CONTINUING WITH COMETS
TALLY ENTRIES 621-630
|621. COMET PANSTARRS C/2015 O1 Perihelion: 2018 February 19.04, q = 3.730 AU
The initial comet that I'll list as I go back on-line with my newly-renamed comet observing effort is something I actually added to my tally over three weeks ago. However, since I like these tally pages to be "decadal," i.e., encompassing even groups of 10, this will be the one that starts it off.
This is one of the many comet discoveries by the Pan-STARRS program in Hawaii that went on-line in 2010, and which at this time can be considered the premier near-Earth asteroid- and comet-hunting survey program in the world. This is, somewhat curiously, the 100th comet discovered by Pan-STARRS (of 155 comet discoveries at this writing, a number that is rapidly increasing all the time). Most of the Pan-STARRS comet discoveries are far too faint for me to observe, or even bother attempting, although the second discovery of the program, C/2011 L4, which was the first one from the program I observed (no. 504), has been the brightest comet of this decade thus far, at least as far as the northern hemisphere is concerned. This latest comet is only the 13th Pan-STARRS comet that I have observed thus far, and indeed there are only nine more that I've even attempted.
Pan-STARRS discovered this comet -- then a relatively dim object of 19th magnitude -- on July 19, 2015, only four days before the 20th anniversary of my discovery of Comet Hale-Bopp C/1995 O1 (no. 199), and just as I was putting the final touches on finishing my autobiography. The initial similarities between the two comets seemed especially remarkable, beginning with the "5 O1" part of their respective discovery designations; this comet's discovery location in southern Capricornus was only a little over 20 degrees east-northeast of Hale-Bopp's discovery location in Sagittarius. The initial calculations also suggested that this comet was at similar distances from the sun and Earth as Hale-Bopp was at the time of its discovery, which suggested in turn that this is a moderately bright comet, intrinsically. Finally, the initial published orbit indicated a perihelion passage in early February 2017 at a heliocentric distance of 1.04 AU, which suggested, if not necessarily a "Great" comet, at least a comet that might become relatively easily visible to the unaided eye, and with good viewing geometry from the northern hemisphere. I speculated a bit on this possibility in my autobiography, although clearly things were too preliminary at that point to make any definitive statements.
Alas, it was not to be. Within a month it was clear that perihelion passage would take place at least a year later than that, at a much larger heliocentric distance. The heliocentric and geocentric distances at discovery (8.42 and 7.42 AU, respectively) were even greater than those initially indicated, although these in turn did verify that the comet is, intrinsically, a bright one. Unfortunately, with the much larger viewing distances involved this rendered any chances of even a somewhat bright comet essentially down to zero.
Comet PANSTARRS is traveling in a fairly steeply-inclined retrograde orbit (i = 127 degrees) and was at opposition (at a heliocentric distance of 4.31 AU) this past June 18. I made my first (unsuccessful) attempt in mid-May, but when I attempted it again on the evening of June 13 I suspected it as an extremely faint and tiny object of magnitude 14 1/2, which I was able to verify as indeed being the comet over the next half-hour due to its motion.
The comet is currently located in southern Hercules a little over three degrees southeast of the star Delta Herculis, and is traveling due westward at a current rate of about 20 arcminutes per day, although this slows down to 10 arcminutes per day by the end of August, at which time it will be located 3 1/2 degrees west of the star Beta Herculis. It reaches its stationary point in early October, when it will be located 3 1/2 degrees west of the star Gamma Herculis (and two degrees north of the Hercules galaxy cluster, Abell 2151), after which its motion turns eastward, although by this time it will be starting to be low in the northwestern sky after dusk. Throughout this entire time the comet will likely remain quite faint, although it does seem to have brightened slightly since I first picked it up; nevertheless, it will still probably gain at most just a few additional tenths of a magnitude in brightness.
Comet PANSTARRS is in conjunction with the sun (40 degrees north of it) in late November, and not too long thereafter becomes accessible in the northeastern morning sky before dawn. At the beginning of 2018 it will be located 1 1/2 degrees due north of Beta Herculis and traveling slightly eastward of due north at 10 arcminutes per day; this rate increases over time as the comet turns more towards due north and then eventually to the north-northwest. At the time of perihelion passage it will be traveling through the "keystone" of Hercules at 20 arcminutes per day and will be located two degrees southwest of the large globular cluster M13; by then it should be at least half a magnitude brighter than it is now, perhaps somewhere between magnitudes 13 1/2 and 14. The comet continues its northwesterly trek after that, crossing into northeastern Bootes in late March and passing north of declination +50 degrees at the end of that month, and then skirting parts of southwestern Draco before entering eastern Ursa Major shortly after mid-April. It is closest to Earth (3.23 AU) in early April, at opposition during the latter part of that month, and at its maximum northerly declination (+57 degrees) in early May; throughout this time it should be near its peak brightness, perhaps near magnitude 13 1/2.
Now traveling towards the west-southwest, Comet PANSTARRS crosses the Big Dipper's "handle" between the stars Zeta ("Mizar") and Epsilon ("Alioth") Ursae Majoris shortly after mid-May, and in fact passes just 15 arcminutes south of the latter star on May 21. Its motion turns more and more towards the southwest, and it passes one degree east of the star Chi Ursae Majoris in early July. Due to both increasing faintness as well as getting lower in the northwestern evening sky, I will probably lose it sometime around that time.
At this time my life is pretty much as described in my July 6 personal statement. Shortly before I picked up this comet I had returned from the 7th SpaceFest conference that was held in Tucson, Arizona, where I had been invited to speak on the "Planetary Defense" panel on the last day (and where I encountered the young lady from Kosovo whom I referred to at the end of my statement). Shortly before that, on May 29 my nephew Jeremy (son of my older brother Barry) and his wife became the parents of a baby girl, Claire, and thus I now have a grand-niece. It will be interesting to see what kinds of changes and goings-on might take place in my life during the year or so that I will be following this comet; I can't help but notice that I will "celebrate" my 60th birthday (ugh!) right around the time that it is brightest. Life goes on, as the comets continue . . .
INITIAL OBSERVATION: 2017 June 14.21 UT, m1 = 14.5, 0.2' coma, DC = 8 (41 cm reflector, 229x)
UPDATE (December 27, 2017): Following its conjunction with the sun, by the latter part of December 2017 Comet PANSTARRS had reappeared in the morning sky, as expected. It has brightened slightly since its pre-conjunction appearance but still appears as a small and moderately condensed object a bit brighter than 14th magnitude. I expect that, during the coming weeks, it will more-or-less follow the above scenario.
MOST RECENT OBSERVATION: 2017 December 23.52 UT, m1 = 13.8, 0.5' coma, DC = 4-5 (41 cm reflector, 229x)
As fate would have it, I was able to sneak one more comet into my tally before "going live" with the re-worked Earthrise web site and with "Continuing With Comets." This newest comet is somewhat of an old friend; it was discovered by Mike Van Ness in September 2005 (apparently after an outburst caused by an earlier fragmentation of its nucleus) during the course of the LONEOS program in Arizona, and I obtained a handful of observations of it then as a faint object (no. 381). During its subsequent return in 2011 I observed it as a part of "Countdown" (no. 485) and followed it for 4 1/2 months, although it remained faint, never getting much brighter than 14th magnitude; the secondary fragment that I commented on during the comet's "Countdown" entry remained much too faint for me to detect. Since 2011, a somewhat distant approach to Jupiter (1.17 AU) in October 2014 has decreased the perihelion distance to the present value and shortened the orbital period to 6.12 years. For whatever it's worth, 213P becomes the seventh comet that I have observed at its discovery return and at both of its next two subsequent returns.
The viewing geometry at the current return is rather favorable, but as April of this year approached and there had not been any announced recovery of the comet, I became curious as to whether or not it still existed -- the fragmenting event in 2005 having led to its eventual demise -- or if in fact it had somehow simply been missed (a moderately high southerly declination of -33 degrees perhaps being a factor), especially when ephemeris predictions were suggesting it might almost be bright enough for visual detection. I ended up making a visual recovery attempt on the morning of April 27, but didn't see anything. I would later learn that the comet had been recovered just a few days earlier, on April 22 by Kevin Hills at the Tacande Observatory at La Palma in the Canary Islands; the reported brightness was close to 18th magnitude.
I didn't look for Comet Van Ness during May, suspecting it was likely too faint for any worthwhile attempts, but I began looking for it again during June, especially after reading reports and seeing images that suggested it had brightened quite a bit. I finally suspected it on the morning of June 29, although it was in a somewhat crowded star field, and I was having to contend with smoke from a distant forest fire affecting my sky conditions; under better conditions, and with the comet in a better star field I easily confirmed it the following morning as as rather vague and diffuse object near magnitude 13 1/2.
The comet is presently located in south-central Sagittarius approximately three degrees southeast of the star Zeta Sagittarii (the southwestern star of the "handle" of the "teapot") and is traveling towards the west-northwest at 12 arcminutes per day. It is at opposition on July 8 and is closest to Earth (1.053 AU) ten days later, during which time its motion is turning more northerly, and it passes within 40 arcminutes southwest of the above star (and one degree northeast of the globular star cluster M54). Afterwards, it travels northward through the "handle," being at its stationary point on August 15 and then turning northeastward, passing half a degree south of the star Omicron Sagittarii in mid-September and a similar distance south of the star Pi Sagittarii a week later, and remaining in northeastern Sagittarius until near the end of October. It is probably close to its maximum brightness right now, possibly gaining a couple of tenths of a magnitude by late July and early August, but probably fading beyond the range of visual detectability not too long after perihelion passage.
More than likely, this will be the last return at which I obtain observations of 213P/Van Ness. The viewing geometry at the next return, in 2023 (perihelion mid-November) is not especially good, and while an approach to Jupiter of 0.57 AU in October 2026 will decrease the perihelion distance to 1.93 AU, neither of the next couple of returns are all that favorable, and by the time of the second one (2036) I am quite certain I will have "retired" from comet observing, anyway.
CONFIRMING OBSERVATION: 2017 June 30.30 UT, m1 = 13.4, 1.6' coma, DC = 2 (41 cm reflector, 229x)
In the late 19th and early 20th centuries astro-photography was coming into its own, and among many other things most of the brighter main-belt asteroids were discovered then -- at such a rate that one astronomer of that era referred to them as the "vermin of the skies" (although the discovery rate of asteroids then was only a small fraction of what it is today). One of the more prolific asteroid discoverers of that era was the German astronomer August Kopff, who was a student, and later professor, at Heidelberg University, earning his Ph.D. there in 1906. Overall he discovered 68 asteroids as well as two comets, both in 1906, with one of these being the periodic comet now known as 22P/Kopff which I've observed on several returns, including my fourth return in 2009 as a part of "Countdown" (no. 448) and more recently in 2015 (no. 572).
One of Kopff's earlier asteroid discoveries was an object he found on February 21, 1906, and which passed perihelion the following January. It was found to be traveling in a low-eccentricity (0.16) orbit with an orbital period very close to five years, and recent studies have indicated that it is approximately 113 km (70 miles) in diameter. The asteroid was assigned the permanent number (596) and Kopff named it Scheila, in honor of a British student and acquaintance of his at the University.
For over a century after its discovery Scheila behaved normally for a main-belt asteroid, and was regularly observed when near opposition. However, on December 11, 2010, Steve Larson with the Catalina Sky Survey in Arizona reported that Scheila has apparently experienced a comet-like outburst, being approximately one magnitude brighter than the ephemeris prediction and exhibiting an extended coma roughly 2 by 5 arcminutes across. Other observers soon confirmed Scheila's cometary appearance, and an examination of earlier Catalina images suggested that the outburst had occurred around the beginning of December, although even during November it was running slightly brighter than predicted.
|(596) SCHEILA FOLLOWING ITS OUTBURST IN DECEMBER 2010. Left: Imaged by Martin Mobberley in England, December 13, 2010. Used with permission. Right: Image obtained with the Hubble Space Telescope by David Jewitt (UCLA) and Max Mutchler (Space Telescope Science Institute) December 27, 2010. Image courtesy NASA/ESA.|
After reading of Scheila's outburst I successfully located it during the early morning hours of December 12, when it was located a few degrees north-northeast of the "head" of the constellation Leo; it appeared slightly fainter than magnitude 13 1/2, and although I couldn't quite convince myself I was seeing any kind of coma, there did seem to be a tiny hint of "fuzziness."
Scheila seemed a few tenths of a magnitude brighter when I next saw it six mornings later, but by then its appearance was completely stellar -- indeed, I never again saw any associated diffuseness that was anywhere near convincing. Overall, it continued to brighten slightly as it approached opposition at the beginning of February 2011, and was near 13th magnitude around that time -- reasonably consistent with the ephemeris prediction. It began fading thereafter -- again, consistent with its ephemeris-predicted brightness -- and I followed it until the evening of June 20, by which time it had faded to 15th magnitude and was getting rather low in the western sky after dusk.
Following its outburst Scheila was, obviously, extensively studied by both numerous ground-based telescopes and by space-based platforms like the Hubble Space Telescope and the Swift Gamma-Ray Burst Mission. An analysis of all this data indicates that Schelia's coma was made up entirely of dust, i.e., no gaseous emissions were present, and this in turn suggests that the outburst was almost certainly due to an impact from a previously-unknown asteroid some 35 meters in diameter.
Such an explanation would suggest that future outbursts would be quite unlikely, yet I have continued to monitor Scheila on a semi-regular basis ever since, usually about once a month or so during the months around opposition. Following its conjunction with the sun in early October 2011 I picked it up again in the morning sky shortly before the end of December as a stellar object slightly brighter than magnitude 14.5, and I observed it on a handful of occasions up through late May 2012 when it had just passed through perihelion and was also near opposition; at that time it was 12th magnitude. I did not observe it any further during that viewing season, in significant part because, as I have indicated in "Counting Comets" and elsewhere, I was dealing with the breakup of my relationship, and for a while almost lost interest in observing. I finally picked it up again in late September 2013 when it was near opposition and magnitude 13 1/2, and observed it on a handful of occasions up through late December, by which time it had faded to 15th magnitude.
In 2014 I picked up Scheila for the first time in early October, when it was just brighter than 15th magnitude. By mid-November it has brightened by a full magnitude as it approached its opposition at the end of that month; meanwhile, it was also approaching aphelion, which took place on November 17 at a heliocentric distance of 3.409 AU. I obtained my final observation of the 2012 "return" on the evening of November 15, when it was 41 hours away from aphelion. I have continued to follow Scheila since that time, but those observations are described in the following entry.
Ever since I first observed Scheila following its outburst in December 2010 -- during which time I included it on the "update" pages of "Countdown," at least through the end of that particular viewing season -- I have devoted considerable thought as to whether or not it I could legitimately consider it a "comet" for tally purposes. Some of the earlier reports do in fact describe it as a "main belt comet" (although the term "active asteroid" has become more in vogue since that time), however once it became clear that the 2010 outburst was almost certainly due to an impact as opposed to any kind of intrinsic activity, Scheila's inclusion as a "comet" seemed rather questionable. In late 2014 as I was working on my autobiography I gave heavy consideration to Scheila, as well as to a couple of other "asteroids" I have observed that have exhibited cometary behavior, as to whether or not I could consider them as "comets" for tally purposes (and with the thought in mind that the IAU Committee on Small Body Nomenclature had not assigned them "dual nature" status); while I did determine that a legitimate case could be made for including the other two objects -- (3200) Phaethon and (3552) Don Quixote (both of which I discuss in my "special note" in the "Continuing with Comets" main page -- I concluded that I could not make a strong enough argument for including Scheila as such.
However, as I also point out in that "special note," the object provisionally designated as P/2010 A2, which was discovered in January 2010 by the LINEAR program in New Mexico, has also been determined as being the result of any impact between two asteroids. It was recovered as a very faint and completely stellar object earlier this year, and was assigned the cometary designation P/2017 B5, despite the nature of the activity it exhibited seven years ago and its current appearance. I pointed out in my "special note" that, if the IAU's Committee on Small Body Nomenclature were to assign a permanent periodic comet number to this object, then an argument could be made that any object that exhibits cometary activity, regardless of the mechanism that produced that activity, can be considered a "comet" for tally purposes, even if its true nature is closer to that of an asteroid.
And, indeed, this is now what has happened. In the July 2017 batch of the Minor Planet Circulars, the object originally designated as P/2010 A2 has now been assigned the permanent periodic comet number 354P. I thus am now adding Scheila to my comet tally retroactively, with my first observed "return" (which contained the actual outburst) constituting this entry, and the current return constituting the following entry.
INITIAL OBSERVATION: 2010 December 12.32 UT, m1 = 13.8, <0.1' coma, DC = 8.5 (41 cm reflector, 70x)
FINAL OBSERVATION: 2014 November 16.22 UT, m1 = 13.8, 0.0' coma, DC = 9 (41 cm reflector, 70x)
I discuss this object's discovery, observational history, 2010 outburst, my early observations, and my reasons for adding it to my comet tally retroactively in the previous entry. I also discuss there how I obtained my final observation of that "return" only 41 hours before aphelion. I didn't wait long to get started on the new return; I obtained my next observation only two nights later, i.e., on the evening of November 17, 2014, when it was only seven hours past aphelion; it appeared completely stellar at slightly brighter than 14th magnitude, and was located in central Taurus five degrees northeast of the Hyades star cluster.
As I had been doing ever since it underwent its outburst, I have continued to monitor Scheila on a semi-regular basis ever since it passed through aphelion, usually once a month or so during the timeframe surrounding opposition; as has continued to be true ever since the outburst subsided, my measured brightnesses have always been within two or three tenths of a magnitude of its ephemeris prediction. It was at opposition near the end of November 2014 and I followed it until early February 2015, by which time its brightness had dropped to magnitude 14 1/2. Following conjunction with the sun in late June 2015 I picked it up again (at magnitude 14 1/2) in early November and followed it through late May 2016, by which time its brightness was again near magnitude 14 1/2; when near opposition in early February it was near magnitude 13 1/2.
After its conjunction with the sun in early October 2016 I picked up Scheila for the first time during the current viewing season on the morning of February 25, 2017, as a stellar object slightly fainter than magnitude 13 1/2. It brightened steadily after that as it approached perihelion in mid-May and opposition at the end of that month; I consistently measured brightnesses near 12th magnitude between mid-May and mid-June. It has started to fade somewhat now, and was 13th magnitude when I most recently observed it a couple of nights ago.
Scheila is presently located in the "head" of the constellation Scorpius, 1 1/2 degrees north of the star Pi Scorpii (the southernmost of the three stars that mark the "head); it is traveling almost due southward at a slow five arcminutes per day and reaches its stationary point on July 17 at which time its motion turns toward the southeast, passing half a degree northeast of the above star around July 28 and half a degree south of the star Tau Scorpii on September 7. It passes less than ten arcminutes north of the globular star cluster M62 on September 25, by which time it will have faded to 14th magnitude, and thereafter travels due east across eastern Scorpius at approximately 20 arcminutes per day, crossing into western Sagittarius on October 27 and becoming lost in the rich Milky Way star fields as it sinks lower into the southwestern sky.
Scheila is in conjunction with the sun in early February 2018 and begins emerging into the morning sky around April; it is at opposition in late September, when it will be near magnitude 13 1/2 and located in southwestern Cetus (passing half a degree north of the bright star Beta Ceti, or Diphda, during the middle of that month). After disappearing into evening twilight in early 2019 it is again in conjunction with the sun in late April of that year; it emerges into the morning sky around July, and should be between magnitudes 13 1/2 and 14 when it goes through aphelion in late November shortly before it is at opposition. As it was when it was at the previous aphelion, it will then be located in central Taurus a few degrees north-northeast of the Hyades.
Provided that I remain active in observing that long -- and my current expectations are that I likely will -- then I will probably continue to monitor Scheila up through its next perihelion passage (late May 2022) and quite possibly for at least another year or two beyond that. I honestly do not expect any repeats of the outburst in underwent in 2010 -- but, one never knows . . .
Scheila's retroactive addition to my tally induces a couple of retroactive changes into my cometary statistics and notable happenings. I commented in my statistical analysis of comets 1-600 that I observed a record number of comets -- 38 -- during the year 2015; with Scheila now being a comet for tally purposes, that total is now 39. It also means that I have now already recorded my 7000th visual comet observation; that distinction goes to the observation I made of Comet PANSTARRS C/2015 ER61 (no. 611) on the morning of June 30, 2017.
INITIAL OBSERVATION: 2014 November 18.28 UT, m1 = 13.8, 0.0' coma, DC = 9 (41 cm reflector, 70x)
FIRST "POST-TALLY ADDITION" OBSERVATION: 2017 July 13.19, m1 = 13.1, 0.0' coma, DC = 9 (41 cm reflector, 70x)
By long-standing tradition, and for obvious reasons, the IAU has limited names on comets to three different discoverers. Even so, some of the resulting comets' names have been rather unwieldy and tongue-twisting; a glance through a list in comet catalogues, or even the list of comets I observed in my earlier years, bears this out. Over the past couple of decades, and especially as more and more comet discoveries began to be made by teams, the IAU has made a strong effort to limit the number of different names on a comet to two. Nowadays, with the various surveys patrolling the skies and finding very faint comets, two independent discoveries of any given comet are rather rare, and thus only a relative few of the comet discoveries over the past decade or so even have two names.
With this particular comet, however, the usage of three different names was probably unavoidable. It was discovered by the Pan-STARRS program in Hawaii on January 23, 2016, however once enough positions had been obtained so that a reasonable preliminary orbit could be calculated, astronomers determined that it had already been discovered, not once, but twice before: the Mount Lemmon survey in Arizona had discovered it on November 2, 2015, whereupon it had been assigned the designation 2015 VL62, and an amateur astronomer, Bill Yeung, had discovered it (via a remotely operated telescope in New Mexico) on December 18, 2015, whereupon it had been assigned the designation 2015 YY6. Neither of these two earlier discoveries had been followed well enough for a linkage to be made or for a reliable orbit to be computed until after the Pan-STARRS discovery.
I've discussed the Mount Lemmon and Pan-STARRS programs in earlier entries in either "Countdown" or "Counting Comets." Bill Yeung (full name William Kwong Yu Yeung) was born in Hong Kong but currently resides in Canada, and has operated remotely controlled telescopes at private observatories in Alberta, Arizona, and New Mexico. He has discovered over 2000 asteroids that have received permanent numbers -- which, including the various surveys, currently puts him in 14th place on that overall list. In September 2002 he discovered a faint object provisionally designated as J002E3 that was at first thought to be an asteroid, but which has apparently turned out to be the S-IVB third stage of the Saturn V rocket that launched the Apollo 12 mission. Yeung has one other comet discovery, also made in 2002: a short-period comet, now designated 172P/Yeung, that has an orbital period of 6.8 years. This particular comet remains very faint and I have never attempted it; it most recently returned to perihelion in March 2017.
Except for its unusually long name, Comet C/2015 VL62 is otherwise one of the many faint, nondescript, large-q long-period comets that show up in my tally quite regularly. It is a first-time visitor from the Oort Cloud, and is traveling in an orbit with an inclination of 166 degrees, i.e., the orbit is inclined only 14 degrees with respect to the ecliptic, but is retrograde. After being in conjunction with the sun in late March 2017 it began emerging into the morning sky, and I made my first attempt in late May and a handful of additional attempts during late June; I occasionally thought I might be seeing an extremely faint "something" but I could never convincingly see anything definite to my satisfaction. On my first attempt of the current dark run, in the early morning of July 18, I suspected a very faint, small, slightly diffuse object a bit fainter than 14th magnitude, and over the course of the next half hour was able to verify my suspect as being the comet via its motion.
The comet is currently located in eastern Pegasus five degrees east of the star Alpha Pegasi (Markab), the southwestern star of the "Great Square" of Pegasus. It is traveling slightly southward of due west, presently at a little over half a degree per day, and passes two degrees south of the above star on July 26. Its apparent motion continues to accelerate as it passes half a degree south of the star Xi Pegasi on August 1 and a similar distance north of the star Zeta Pegasi two days later, by which time its speed will have increased to 50 arcminutes per day. The comet is at opposition on August 17 and is nearest Earth (1.74 AU) four days later; at that time it will be still be located in Pegasus (albeit in the southwestern corner of that constellation) but crosses into northwestern Aquarius on August 26; it will then be traveling at its peak speed of one degree per day and should be near its peak brightness, perhaps half a magnitude or so brighter than it is now.
At the time of its perihelion passage the comet will still be in northwestern Aquarius, some four degrees southwest of the star Alpha Equulei. As it pulls away from both the Earth and the sun it should begin fading and slowing down, and its motion turns more and more southerly; it crosses into southeastern Aquila on September 5 and remains within that constellation before finally crossing into northeastern Sagittarius on October 8. Sometime during this period it will likely have become too faint for visual observations. The planetary perturbations it has encountered during its passage through the inner solar system have placed it into a slightly hyperbolic orbit, and it will eventually leave the solar system altogether.
INITIAL OBSERVATION: 2017 July 18.32 UT, m1 = 14.3, 0.4' coma, DC = 6-7 (41 cm reflector, 229x)
In today's era of comprehensive sky surveys it is not unusual -- indeed, it is pretty much the norm -- for any long-period comets I observe to be discovered several months, and often a year or more, before they become bright enough for me to detect visually. Comets that are already bright enough for visual detection at discovery are rather rare these days, especially comets that are somewhat bright. But that is exactly what happened with this particular comet.
The comet was first detected on July 19, 2017, in images obtained during the course of the All-Sky Automated Survey for Supernovae (ASAS-SN) program that is operated by Ohio State University. ASAS-SN operates two "clusters" of four automated 14-cm telescopes, one of these being located at Mount Haleakala in Hawaii, the other at Cerro Tololo Inter-American Observatory in Chile. As its name implies, ASAS-SN surveys the entire sky on almost a nightly basis looking for supernovae in other galaxies, and has been very successful at this, having currently discovered over 500 supernovae since going on-line in mid-2013, including what appears to be the most luminous supernova ever observed. C/2017 O1, which was reported as being 15th magnitude when it was first detected by the Cerro Tololo telescope cluster, is its first comet discovery.
Shortly after its discovery, the comet was placed on the Minor Planet Center's Possible Comet Confirmation Page under the designation "ASASSN1." I immediately made plans to attempt observing it, but unfortunately I was clouded out for the next few mornings by our typical summertime monsoon weather here in New Mexico. Finally, on the morning of July 24, under somewhat mediocre sky conditions -- just a few hours after a very heavy rainstorm -- I was able to make an attempt, and easily saw the comet as a large, vague, and diffuse object 5 arcminutes in diameter and 11th magnitude.
Being at an elongation of 85 degrees and easily accessible from both hemispheres at the time of its discovery, and being as bright as it was, it is natural to ask why this comet wasn't discovered sooner -- indeed, it has been rather easily accessible from the southern hemisphere since about April. An answer might be provided by subsequent ASAS-SN images, which seem to show a dramatic increase in brightness shortly after discovery; this may also help explain why I (and other visual observers) found it so bright. It is possible -- especially if this is an "old" comet that has previously visited the inner solar system in the distant past -- that it is just now "turning on;" there is precedent for this type of behavior in other observed comets. Of course, it is also possible that it is presently undergoing an outburst and that its brightness will soon subside. The only way to tell will be to see how it behaves during the days and weeks to come.
In any event, at least according to the preliminary orbit available at this writing (which shows that the comet is traveling in a direct orbit with an inclination of 40 degrees), the viewing geometry during the near- to intermediate-term future is very favorable for the northern hemisphere. It is currently located in northwestern Eridanus three degrees northwest of the star Eta Eridani and is traveling towards the northeast at just over half a degree per day; it enters southwestern Taurus on August 20, passing 2 1/2 degrees west of the star Lambda Tauri on September 6 and six degrees west of the Hyades star cluster five days later. By this time its motion will have turned more northerly and increased to over 50 arcminutes per day; it passes 5 1/2 degrees east of the Pleiades star cluster (M45) on September 21 and crosses into southeastern Perseus six days after that. At the time of perihelion passage it will be located in the northeastern portion of that constellation 4 1/2 degrees east of the star Lambda Pesei; at that time its motion will be almost due northward at close to 70 arcminutes per day. Three days after perihelion the comet is closest to Earth (0.72 AU), at which time it crosses into southwestern Camelopardalis.
Continuing its northward trek, the comet becomes circumpolar for mid-northern latitudes by the end of October, and travels north of declination +80 degrees on November 17, at which time it crosses into the constellation Cepheus and its motion will have slowed down to half a degree per day. The comet remains north of declination +80 degrees until February 8, 2018, and reaches a maximum just south of +86 degrees on December 9, when it will be a little over three degrees south of the North Star, Polaris. After exiting the +80 degree region it travels southeastward through Camelopardalis for the next two months, passing 20 arcminutes northeast of the bright spiral galaxy NGC 2403 on March 30, and remains in northern circumpolar skies until near the end of April.
As for the comet's brightness prospects . . . Based upon the brightness I measured on my first observation, and under the assumption that the comet behaves more-or-less "normally" from that point, it should reach 10th magnitude in August and 9th magnitude in September, and be close to 8th magnitude around the time of perihelion and closest approach to Earth. After that it should fade slowly, being close to 10th magnitude at the end of 2017 and fading beyond the range of visual observations by perhaps sometime in March 2018. If, as some of the initial images suggest, it is currently in the midst of a rapid brightening, then it may become brighter than the above scenario suggests, although I doubt if it will reach naked-eye brightness. On the other hand, if it is undergoing an outburst right now, it may well be fainter than the above scenario suggests, and possibly could even disintegrate at some point in the not-too-distant future. Only time will tell . . .
While it has received a formal designation, as of this writing Comet C/2017 O1 has not yet been formally named. My understanding is that the IAU's Committee on Small Body Nomenclature is still discussing what name to assign to the comet -- which presumably would apply to any future discoveries by the ASAS-SN program. I will update this entry when a name is assigned (and perhaps by then we will also have a better understanding on the comet's future behavior).
For whatever it's worth, I note that this is my 450th separate comet. As I indicate in my introductory comments to "Continuing with Comets," my next goal is to reach my 500th separate comet. My 400th separate comet was Comet Jacques C/2014 E2 (no. 540), which I added to my tally in March 2014; this would seem to suggest that I will reach separate comet no. 500 sometime in late 2020 or in early 2021. It's worth mentioning that three of my additions to this list since my 400th comet were previously-observed "asteroids" that I added to my tally retroactively (such as (596) Scheila), and it is conceivable that one or more of my forthcoming entries could also be due to retroactive additions.
INITIAL OBSERVATION: 2017 July 24.45 UT, m1 = 11.0, 5' coma, DC = 2 (41 cm reflector, 70x)
UPDATE (August 31, 2017): The International Astronomical Union has now officially assigned the name "ASASSN" (pronounced "assassin") to this comet.
The most recently available orbit is quite similar to the initial orbit, and the above location scenario remains basically unchanged. The period of time during which the comet remains north of declination +80 degrees is November 15, 2017 through February 11, 2018, with a maximum declination of +86 3/4 degrees occurring on December 8, around which time it will be located 2 1/2 degrees from the North Star, Polaris. The close approach to the galaxy NGC 2403 takes place on March 29, 2018, with the minimum separation now increased to 50 arcminutes.
As for the comet's brightness, that still remains problematical. Its apparent rapid brightening near discovery seems to have continued, and the comet was at 10th magnitude during the last days of July. However, it has not really brightened since that point, in fact it seems to have faded slightly, although it is also beginning to appear more condensed, and CCD images I've seen are showing a stubby tail (which I have not yet detected visually). If it brightens "normally" from its present brightness it should peak near 9th magnitude, possibly slightly brighter, when near perihelion and closest approach to Earth, and should remain visually detectable for perhaps one to two months after the start of 2018.
MOST RECENT OBSERVATION: 2017 August 29.39 UT, m1 = 10.3, 5' coma, DC = 5 (41 cm reflector, 70x)
I have just recently returned from a 3 1/2-week-long road trip to various places throughout the western U.S. My travels initially took me to Monterey, California, where I attended and spoke at the Starship Congress put together by my colleagues at Icarus Interstellar; reconnecting with these colleagues after my recent era of darkness is helping me to gain some positive perspectives on my future activities, and I foresee additional involvement on my part in this endeavor (although I'm still working on just what this will entail). After the Starship Congress I spent the next week and a half "bumming around" northern California and southern Oregon; among the places I visited were Lassen Volcanic and Crater Lake National Parks and the Malheur National Wildlife Refuge, and I spent one night at the historic Frenchglen Hotel in Frenchglen, Oregon.
|PLACES I VISITED DURING THE "BUMMING AROUND" PHASE OF MY RECENT ROAD TRIP. Left: Crater Lake National Park, Oregon. Right: The beach at Carl G. Washburne Memorial State Park, along U.S. Highway 101 north of Florence, Oregon, where I sat and contemplated the universe for a while.|
|After completing the "bumming around" portion of my trip, I arrived in Corvallis, Oregon shortly after mid-August. My younger son Tyler relocated there earlier this year; while he possesses a Master's Degree in Music, he has decided to pursue an additional degree in Electrical Engineering, and is now enrolled and taking classes at Oregon State University. In addition to visiting Tyler, I was there to observe the total solar eclipse on August 21.
Ever since I first began traveling to solar eclipses -- my first total eclipse was the one on February 26, 1979 -- I have attempted to observe any comets that might be near the sun during totality, an endeavor which, thus far, has been entirely unsuccessful. With the launch of the SOHO spacecraft in late 1995 and the detection of over 3000 comets -- the large majority of which are Kreutz sungrazers (which I discuss in the "Countdown" entry for Comet Lovejoy C/2011 W3 (no. 500)) -- in the LASCO C3 (outer) and C2 (inner) coronagraphs since that time, the possibility of success at some point would seem to be at least conceivable. For this eclipse I collaborated with Karl Battams, the "comet person" for the SOHO mission (and who manages the "Sungrazer Project" web page), in an attempt to observe any comets that might be detected in LASCO images. In addition to weather and equipment considerations, for such a project to be successful the timing has to be almost perfect, i.e., there has to be a reasonably bright comet within a few hours before its perihelion passage at the instant of totality. I estimated that the odds of success were never greater than about 5%.
As things turned out, there was, not one, but two, Kreutz sungrazing comets that appeared in the LASCO C3 images prior to totality, however these appeared about 18 hours too soon. They were brightest -- about 6th magnitude -- in the C3 images about 18 hours before totality, and then began to fade as they disintegrated during their approach to perihelion; while they were still faintly visible when they appeared in the C2 images about three hours later, they disappeared shortly thereafter.
With my primary reason for observing the eclipse no longer in play, I resolved primarily to just enjoy the eclipse, and hopefully get one or two decent photographs with the DSLR camera I purchased three years ago. The sky was completely clear from Corvallis, however the duration of totality was quite short, only 1m 40s. I did get a decent but brief visual view of totality, including seeing the star Regulus close to the sun in 10x50 binoculars, but unfortunately the shutter release on my camera jammed, and I was unable to get any decent photographs.
|ABOVE: The two Kreutz sungrazing comets that appeared in the LASCO C3 images prior to the August 21 solar eclipse. The two comets are widely disparate in appearance; the left one is long and elongated, the right one is almost a point source. The trio of stars that the comets pass by are (top to bottom) 18 Leonis, 19 Leonis, and R Leonis. Upper image is 19:54 UT August 20 (20 hours before totality), the lower image is 23:06 UT (17 hours before totality). Images courtesy NASA/ESA. RIGHT: Wide-field image of totality from Corvallis, Oregon. Photograph courtesy Vickie Moseley, who observed the eclipse with Tyler and me.|
|It was then time for the return drive home, which among other things included a fairly brief stop at Arches National Park in Utah. I arrived home late in the afternoon of Sunday, August 27.
While I did bring two telescopes with me on the trip, other than during the solar eclipse I ended up not making any observations; most of the time I was not in a location where I could have easily used them in a dark sky, and the two nights when I was so located -- and had indeed planned on making some observations -- the skies were cloudy. When I returned home the moon was already in its first quarter phase, which meant that I only had a few mornings of potential observing left before the approaching full moon would interfere. Fortunately, the summer monsoon -- which tends to begin sputtering around this time of the year anyway -- has been (with one exception) mostly quiet since my return, and I've been able to collect several observations; with more rain being forecast for this coming weekend, and the full moon right afterwards, I am probably about finished for the current dark run. I did, however, manage to add an additional comet to my tally during these few clear nights of observing, and it is one that I had absolutely no expectation of seeing.
This comet, which was originally discovered by the NEAT program in December 2002, is one I have actually seen before, during its subsequent return in 2010 when I observed it during "Countdown" (no. 483). As I remarked during its "Countdown" entry, despite the fact it was rather favorably placed on that return, I was only barely able to detect it as a very faint object of magnitude 14 1/2, and indeed I obtained only a handful of observations of it. As I also recount there, the geometrical conditions at the current return are considerably less favorable, and thus there has been no reason to think I might see it.
The comet was recovered on July 6, 2017, by Larry Denneau and colleagues with the Asteroid Terrestrial-impact Last Alert System (ATLAS) program based in Hawaii. It was located almost four arcminutes from its predicted position, corresponding to a correction of almost eight hours to its predicted time of perihelion passage -- an unusually large amount for a comet that has been observed through two returns -- and the resulting orbital solution required non-trivial gravitational forces. It was reported as being about 18th magnitude, and was not expected to get much brighter this time around.
An image taken by Japanese amateur astronomer Kunihiro Shima on August 22, and posted to Facebook a few days later, shows the comet in apparent outburst near 14th magnitude. Armed with this information, I made an attempt on the morning of August 29, and successfully detected the comet as a small and extremely faint object of 14th magnitude; I detected a slight motion over the course of an hour and a half, and successfully observed it again the following morning.
At this time it is difficult to predict the future behavior of this comet. If, as I suspect, it has recently undergone an outburst, then I would expect fading to set in soon; with the expected rain this weekend and the coming full moon, the two observations I have thus far may well end up being the only ones I obtain. (For what it's worth, the comet seemed less condensed and more diffuse on the second morning.) If, on the other hand, the recent brightening is sustained, then I could end up following it for quite some time. It is presently located at a declination of -34 degrees in central Sculptor some six degrees southwest of the star Alpha Sculptoris and, having just passed through its stationary point in mid-August, is now traveling towards the southwest at 10 arcminutes per day. The comet remains in Sculptor for the next three months, as its motion gradually turns more directly westward; it is at opposition in late September and is nearest Earth (1.88 AU) in early October, at which time it is also at its furthest south (declination -36 1/2 degrees). It passes through its other stationary point in mid-November (when it will be located 2 1/2 degrees east-northeast of the star Mu Sculptoris) and begins direct (eastward) motion, although much of this will be northward. The comet crosses into southwestern Cetus in mid-December and thereafter spends the next four months tracking northeastward across that constellation (although nicking far southeastern Pisces in mid-March 2018 and passing less than five arcminutes south of the star Alpha Piscium on March 13). By the end of that time it will be lost in evening twilight; it is in conjunction with the sun (almost directly behind the sun) in early June, begins emerging into the morning during the latter part of August, and is at opposition again in early March 2019.
I point out in this comet's "Countdown" entry that the next return, in December 2025, is very favorable, with opposition and perihelion occurring almost simultaneously; if the brightness I'm seeing now is exhibited then, then it should be some 2 1/2 magnitudes brighter than it is at present, i.e., close to magnitude 11 1/2. However, I strongly doubt that will happen; I am reasonably certain that we are currently seeing an outburst that will soon subside, and I will have few if any additional observations this time around. Even without an outburst, the expected brightness in 2025 does look favorable at face value -- although I don't know if I'll still be observing comets then -- however, there have been other short-period comets where the current behavior, i.e., far away from its predicted location, with resulting large non-gravitational forces being necessary to resolve the discrepancy, and unexpected brightening, has been associated with the act of disintegrating. Thus, it is within the realm of possibility that there will not be anything to see of this comet in 2025. As always, time will tell.
There are a couple of other interesting astronomical events going on at this time, that have been among the observations I've collected since my return. Comet 29P/Schwassmann-Wachmann 1 (no. 498) has just undergone the largest outburst of its present "return" and is presently near 12th magnitude. Meanwhile, one of the larger Earth-approaching asteroids, (3122) Florence, is currently making a close approach to Earth; it passes 0.047 AU away on September 1. I observed it on the morning of August 30 and could see it even in 10x50 binoculars, at magnitude 8.9.
INITIAL OBSERVATION: 2017 August 29.44 UT, m1 = 14.1, 0.4' coma, DC = 3 (41 cm reflector, 229x)
UPDATE (September 24, 2017): This comet was still faintly detectable at magnitude 14.3 when I attempted it on September 17, although it was also quite vague and diffuse, and near the limit of visibility. It would appear, then, that the recent outburst is being maintained for at least a little while, although I doubt if it remains visible for much longer.
I've commented in various entries, both presently as well as in the previous programs, about the significant number of nondescript, distant long-period comets that appear on my tally. This is, to some degree, a non-trivial by-product of the comprehensive sky surveys that have been on-line for the past two decades. A good example of this phenomenon is a trio of unrelated long-period comets discovered by Pan-STARRS during the (northern hemisphere's) summer of 2016; all three pass perihelion (at heliocentric distances between 2.2 and 2.7 AU) during the middle months of 2018, and I've expected all three to become bright enough for visual observations. Due to their large distances they all should be visually detectable for a significant period of time, although I don't expect any of them to get very bright.
The first comet of the trio that I've picked up, although it was the last one to be discovered, is this one, which was found by Pan-STARRS on September 7, 2016. It was located at a moderately high southerly declination of -38 degrees, and although initially reported as being 18th or 19th magnitude, some of the subsequent reports and images I saw suggested it might be worth attempting. I began doing so in early October and continued to make occasional attempts (as the comet slowly traveled southward to declination -42 degrees and then began to head northward) up through the middle of February 2017. After being in conjunction with the sun (32 degrees south of it) in mid-May the comet began emerging into the morning sky a couple of months later, and I resumed attempts in early August, although for a while these remained unsuccessful.
I made my first attempt after the early September full moon on the morning of September 17 and seemed to have a reasonable suspect, however it was traveling over a pair of faint stars and I was unable to verify this suspect. On the following morning the comet was located in a "clean" position and I clearly detected it as a very faint and somewhat condensed object slightly fainter than 14th magnitude, and thus verified my suspect from the previous morning.
The comet is presently traveling slowly through the "belt" of the constellation Orion, being currently located some 1 1/2 degrees south-southwest of Epsilon Orionis ("Alnilam"), the middle of the "belt stars." It is in a moderately-inclined direct orbit (inclination 58 degrees) and is traveling primarily northward; it reaches its stationary point in early October when it will be located just south of Alnilam, and it passes 2 arcminutes east of that star on October 12. After that the comet continues traveling northward, although it gradually turns more and more westward; it passes half a degree east of Delta Orionis ("Mintaka") -- the westernmost of the "belt" stars -- during the third week of October, and then passes through the northern portion of Orion's "shield" in early December -- at which time it is at opposition -- before crossing into southern Taurus during that middle of that month.
Following opposition the comet continues its northwestward motion through Taurus, being nearest Earth (2.05 AU) in late December and traversing the southwestern portion of the Hyades star cluster during the first week of January 2018. Its motion then turns more directly northerly, being at its stationary point shortly before mid-February, at which time it will be located three degrees east of the Pleiades star cluster (M45). With its motion now turning more and more towards the northeast, the comet crosses into southern Perseus in early March and then into western Auriga in early April, passing two degrees southeast of the bright star Capella in early May and being three degrees east-southeast of that star at the time of perihelion passage. Traveling more and more easterly, it passes north of declination +50 degrees and crosses into northwestern Lynx in early June. The comet is at its farthest north declination -- just south of +53 degrees -- and crosses into western Ursa Major shortly after mid-July, and then spends the next two months traveling westward through that constellation before crossing into western Canes Venatici in late September (and passing nine arcminutes north of the galaxy M106 on the 29th), at which time it is also in conjunction with the sun (47 degrees north of it). Now in the morning sky, the comet tracks almost due eastward, crossing into western Bootes in mid-November and remaining in that constellation for the rest of 2018.
While brightness predictions for any long-period comet are always a bit problemetical, the fact that this comet appears not to be a "new" comet from the Oort Cloud -- having an approximate orbital period of 20,000 years -- suggests that it might perform reasaonably well despite its distance from Earth and from the sun. Based upon the brightness I observed when I first picked it up, it may peak at somewhere between magnitudes 12 and 12 1/2 from late December 2017 through February 2018. It should still be near 13th magnitude when near perihelion and perhaps a half-magnitude or so fainter when it goes through conjunction with the sun a year from now, and will likely fade beyond visual range during the last couple of months of 2018.
In some of the "Countdown" and "Counting Comets" entries I've commented about how productive the months of July and August have been with regard to adding comets to my tally, despite the fact that these are the "monsoon" months here in New Mexico. Over recent years another, perhaps even more remarkable, trend has become apparent: every year since my relocation to 16 Springs Canyon in 1995, I have managed to add at least one comet to my tally during the month of September. The addition of this comet to my tally extends this string for the 23rd consecutive year. And then, less than two days later, I added another comet to my tally this September -- the second comet of the trio I mentioned at the beginning of this entry.
CONFIRMING OBSERVATION: 2017 September 18.43 UT, m1 = 14.2, 0.9' coma, DC = 3 (41 cm reflector, 229x)
UPDATE (January 10, 2018): As it has approached perihelion Comet PANSTARRS has begun exhibiting an extremely dynamic, almost bizarre, ion tail structure that changes quite rapidly in "real time." This behavior calls to mind a couple of historical comets, mainly Comet Morehouse 1908d and Comet Humason 1961e, both of which were very rich in ionized carbon monoxide. Comet PANSTARRS is also very rich in ionized carbon monoxide, and thus appears to be a third member of this rather rare class of comets.This tail structure shows up well in blue-sensitive images but is difficult to detect visually; at best, I have only been able to detect some slightly curved "boundaries" in what otherwise appears as a faint, featureless tail.
Comet PANSTARRS C/2016 R2 as imaged by the Las Cumbres Observatory's station at the South African Astronomical Observatory. LEFT: January 8, 2018 as imaged with blue filter. RIGHT: Combined color image obtained January 9, 2018, by Las Cumbres Observaotry Director Edward Gomez. Note changes in ion tail structure over a 24-hour period.
MOST RECENT OBSERVATION: 2018 January 5.13 UT, m1 = 10.8, 4' coma, DC = 4 (41 cm reflector, 70x)
The second of the "trio" of distant long-period comets on my tally that I mention near the beginning of the previous entry was actually the first to be discovered: Pan-STARRS found it on June 22, 2016, at which time it was an 18th-magnitude object in far northern skies near a declination of +69 degrees. Traveling in an orbit that is almost exactly perpendicular to Earth's (inclination 91 degrees), it has been slowly heading southward ever since, being in conjunction with the sun (69 degrees north of it) in late December 2016 and at opposition in late June 2017. I first began making attempts for it in mid-June, and these were unsuccessful for the next two months, including my first attempt after the early September full moon. However, on the evening of September 18 I was able to detect it as an extremely faint (magnitude 14 1/2) object that moved as expected over the next two hours, and I successfully tracked it for another hour on the following night.
The comet is currently located in central Hercules one degree east of the star Epsilon Herculis (the southwesternmost star of the "keystone"), and is traveling slightly eastward of due south at a little under 20 arcminutes per day. It remains in Hercules, well placed for observations in the evening sky, for the next several weeks, eventually crossing into northern Ophiuchus in late November and passing five degrees east of the star Alpha Ophiuchi ("Rasalhague") in early December. It is in conjunction with the sun (33 degrees north of it) right around Christmastime, and thereafter is better placed for observation in the morning sky. If it brightens normally, it should be close to 13th magnitude by that time.
At the beginning of 2018 the comet is still located in northeastern Ophiuchus, three degrees southeast of the star 72 Ophiuchi, and is traveling towards the southeast (still at a little under 20 arcminutes per day), although this motion turns more directly to the east over the ensuing weeks. It passes 15 arcminutes north of the star cluster NGC 6633 on January 11 before crossing into northern Serpens Cauda three days later, and then a week and a half after that spends three days (the 21st through the 23rd) crossing the southern regions of the large star cluster IC 4756. The comet crosses into northwestern Aquila during the second week of February and spends the next three months in that constellation with its motion turning more directly southward; it is at its stationary point in late April and then crosses into northeastern Sagittarius in early May.
The comet spends the next six weeks crossing southwestward across Sagittarius, entering the "handle" of the "teapot" in early June and passing half a degree southwest of the globular star cluster M54 on June 9 before crossing into Corona Australis during the third week of June, by which time it is traveling at slightly over one degree per day. It is at opposition on June 24, at which time it is also closest to Earth (1.29 AU). Based upon its present brightness, and the fact that it appears not to be a "new" comet from the Oort Cloud (approximate orbital period 30,000 years), the comet should be at least as bright as 10th magnitude, possibly 9th, during this time.
Following opposition, the comet crosses far southeastern Scorpius and enters Ara by the end of June. By the second week of July its declination drops south of -50 degrees and I will lose it, although observers in the southern hemisphere should be able to keep track of it for quite some time thereafter. It crosses through the constellations of Norma and Circinus before entering southeastern Centaurus during the third week of August; it is at its stationary point shortly after mid-September with its motion thereafter turning towards the south-southeast, as it passes 1 1/2 degrees east of the star Alpha Centauri shortly before the end of that month. After that the comet crosses back into Circinus and travels through that constellation and later Apus, passing south of declination -80 degrees during the second week of December and crossing into Octans shortly after mid-month. At the very end of 2018 it passes slightly within four degrees of the south celestial pole and may still be as bright as 12th magnitude; afterwards it spends the first six months of 2019 traveling northeastwards through the constellations of Hydrus, Reticulum, Dorado, Pictor, and Columba, during which time it will likely fade beyond the range of visual detectability. While it does pass north of declination -40 degrees in late April and declination -30 degrees in late June, those parts of the sky are inaccessible from the northern hemisphere during those times of the year, and there is no possibility of my observing it (unless I happen to be in the southern hemisphere then, which I suppose is conceivable).
During the period I have been attempting this comet I have also been attempting the third comet of the "trio," C/2016 N6, and have come close to suspecting it on a couple of occasions. It is presently somewhat low in my northwestern sky during the evening hours, and it is in conjunction with the sun (63 degrees north of it) in early November, and I think there is a reasonable possibility I may be able to add it to my tally by the end of 2017. It travels through northern circumpolar skies in early 2018 and passes within 9 1/2 degrees of the north celestial pole in mid-March, and while I do not expect it to become bright, I should at least be able to complete the "trio."
INITIAL OBSERVATION: 2017 September 19.21 UT, m1 = 14.4, 0.7' coma, DC = 3-4 (41 cm reflector, 229x)
UPDATE (January 25, 2018): After its conjunction with the sun in late December 2017, I picked up this comet as it was emerging into the morning sky a month later, when it was located just one degree southeast of the large star cluster IC 4756. While it has brightened slightly since the last time I saw it in late November, this has been by no more than half a magnitude, and it is now close to a full magnitude fainter than the expectations for this time, upon which the above scenario was based. Thus, while a lot can still happen between now and perihelion (and afterward), the comet may be distinctly fainter than what the above scenario suggests.
MOST RECENT OBSERVATION: 2018 January 25.53 UT, m1 = 13.9, 0.6' coma, DC = 3 (41 cm reflector, 229x)
In early January 1965 two rather faint short-period comets were discovered from the Tsuchinshan, or Purple Mountain, Observatory near Nanking, China. The two comets were located some 25 degrees from each other, and both traveled in somewhat similar orbits -- the biggest differences being the two respective perihelion distances (1.49 AU for the first one vs. 1.77 AU for the second one) and the fact that their respective nodes were reversed, i.e., the ascending node of one comet corresponded to the descending node of the other, and vice versa; however, their respective perihelion points were relatively close to each other. Moreover, both comets were found to have had close encounters with Jupiter near the previous aphelion, and for a while there was speculation that the two comets might be separate fragments of an earlier single comet that had split in two. Additional studies showed, however, that the two comets are completely unrelated to each other, and that their closeness in the sky around the time of discovery, and the similarities in their respective orbital elements, are nothing more than coincidences.
Both comets returned in 1971 and were successfully recovered. The second of the two, Tsuchinshan 2, was the first to be recovered, and has since been assigned the designation 60P; the first one was recovered three months later and has since been assigned the designation 62P. Both have been recovered on most of their subsequent returns since then. I have visually attempted 60P/Tsuchinshan 2 on three different returns, but have been unsuccessful every time; it returns under favorable geometric conditions near the end of next year (and with a somewhat smaller perihelion distance due to another encounter with Jupiter a decade ago) and thus I may finally be able to pick it up then.
I have fared considerably better with my attempts for 62P/Tsuchinshan 1. I first observed it in very late 1984 while it was en route to its perihelion passage early the following year (no. 80); the geometrical conditions were quite favorable and it reached a peak brightness of 10th magnitude. I didn't attempt it during its unfavorable return in 1991, however -- somewhat to my surprise -- I was able to obtain a handful of observations of it (as a very faint and vague object of 13th magnitude) at the mediocre return in 1998 (no. 240).
|The subsequent return in late 2004 was moderately favorable, and I followed it for four months (no. 361), during which it reached a peak brightness of 11th magnitude. During the period of time I was following it, it crossed the Virgo Cluster of Galaxies at the same time that the 48-inch (1.2-meter) Oschin Schmidt telescope at Palomar Observatory was taking images for the "Big Picture" mural that is now featured at Griffith Observatory in Los Angeles, California, and it shows up in the mural as two pairs of blue and green images.
After the subsequent aphelion the comet passed 0.72 AU from Jupiter in August 2009, which decreased its perihelion distance to the present value and shortened its orbital period from 6.63 years to 6.37 years. The geometrical conditions at the subsequent return in 2011 were very unfavorable, and it was not recovered.
|An excerpt of the "Big Picture" mural (featuring the Virgo Cluster of Galaxies) at the Griffith Observatory in Los Angeles, California. Comet 62P/Tsuchinshan 1 is the two pairs of double images (taken through blue and green filters) at lower right (January 18, 2005) and lower left of center (the following night). The large galaxy just right of top center is NGC 4473; the pair of galaxies at lower right are NGC 4458 (top) and NGC 4461 (bottom). Image courtesy Griffith Observatory and CalTech.|
On its current return Comet 62P was recovered on August 10, 2017 by an American amateur astronomer, Jonathan Tuten, utilizing a remotely-controlled telescope at Slooh Observatory in the Canary Islands, and independently three days later by a French amateur astronomer, Francois Kugel, at his private observatory in Dauban, France. I made one unsuccessful attempt for it in mid-September, and then on the morning of October 2 -- one of the last dark mornings before the current full moon -- I successfully spotted it as as a very faint and vague diffuse object near magnitude 13 1/2, and followed it for about an hour.
The comet remains a morning-sky object throughout this return (at least, when bright enough to be visually detectable). It is currently located in central Cancer just a little over a degree south of the Praesepe (or Beehive) star cluster (M44), and is traveling slightly southward of due east at approximately 50 arcminutes per day. It crosses into western Leo in mid-October and spends the next month and a half tracking east-southeastward across that constellation -- passing 2 1/2 degrees north of the bright star Regulus shortly before the end of October and 20 arcminutes south of the star Iota Leonis on November 22 -- before crossing into western Virgo shortly before the end of November. The comet then spends the next several months within Virgo, crossing through the southern portion of the Virgo galaxy cluster in early December, being at its stationary point in early March 2018 (when it will be four degrees west-northwest of the star 109 Virginis), and is at opposition during the third week of April. It is closest to Earth (1.02 AU) in mid-March.
Based upon the brightness it has exhibited at past returns, Comet 62P should reach a peak brightness near 12th magnitude, possibly a little brighter, during November and December. I've suspected a bit of asymmetry in its brightness behavior with respect to perihelion -- like that exhibited by comets like 6P/d'Arrest, although not as extreme -- on a couple of the past returns, and if that is true then the comet may not reach its peak brightness until perhaps December. In any event, while it will probably still be visually detectable after the start of the new year, it will almost certainly have faded beyond visual range well before the time it reaches opposition.
On its way to its next aphelion Comet 62P passes 0.27 AU from Jupiter in April 2020, which will shorten the orbital period down to 6.18 years and the perihelion distance down to 1.26 AU. The next return (perihelion December 2023) is very favorable, with the comet's passing 0.50 from Earth and possibly reaching 9th magnitude. Thus, provided that I'm still active in observing comets, I should be seeing this one at least one more time, even if I do stick to the "retirement schedule" that I alluded to on the main page. Looking further ahead, the comet will pass only 0.015 AU from Mars in early April 2049, but even if I'm still alive (at the age of 91) it is rather unlikely that I'll be seeing that particular event -- I will leave that to future generations of comet observers.
INITIAL OBSERVATION: 2017 October 2.48 UT, m1 = 13.6, 1.0' coma, DC = 1-2 (41 cm reflector, 229x)
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