The discovery of the "second Kracht group"
[This page shows how the term "Kracht2 group" came into being. The Marsden, Meyer and Kracht comet groups were found 2002 from observations with SOHO LASCO. The initial announcement on IAUC 7832 of the Meyer group showed only four members of this new group, but until now (2015 May) more than 100 members have been found. The "new group" announced on IAUC 8340 in 2004 had initially only three comets and I used the name "Kracht2 group" for the "new group". Later Karl Battams used this name for the description of the SOHO comets at the sungrazer site and others used this name also. But no new comets have been found to belong to this "new group". C/2002 R5 had split in two parts when it returned in 2008 and C/1999 R1 is identical with C/2003 R5, so there are still (as of May 2015) only three comets. The expectation from 2004 for a new group did not come true.]
SOHO's images have been posted on its website since 1999 May. Terry Lovejoy was the first internet user to discover a SOHO comet in 1999 August. Five weeks later, he found a non-Kreutz group comet. It was designated C/1999 R1 (MPEC 1999-R19). Brian Marsden wrote (IAUC 7251):
COMET C/1999 R1 (SOHO)
D. A. Biesecker, SM&A Corporation and Goddard Space Flight Center,
reports observations of what is presumably a comet, not a Kreutz
sungrazer, discovered by T. Lovejoy in SOHO/LASCO C3 data and later
also recognized in earlier C2 data. Astrometry and orbital computations
are given on MPEC 1999-R19. Biesecker also provides the following
LASCO magnitudes, reduced using the Hipparcos Input Catalogue:
Sept. 5.47 UT, 6.6; 5.53, 6.5; 5.57, 6.4; 5.61, 6.3; 5.65, 6.2;
5.70, 6.2; 5.78, 6.4; 5.82, 6.4; 5.86, 6.7; 5.90, 6.9; 5.99, 6.9;
6.07, 7.4; 6.15, 7.4. No tail was detected.
Three years later, Rob Matson found another non-Kreutz group comet first in C2 images and later in C3 images. Only one hour after he had posted his find, I wrote:
Congrats! It moves very close to the apparent track of C/1999 R1 with the right speed. So it's certainly related to C/1999 R1 and there could evolve another new group.
The comet was designated C/2002 R5. Brian Marsden wrote (MPEC 2002-S35, IAUC 7984):
C/2002 R5 appears to be related to C/1999 R1, a point first made by R. Kracht;
Finally, Kazimieras Cernis found another non-Kreutz group comet in C2 images of 2003 September 08 and later in C3 images. I wrote:
Congrats Kazimieras! The apparent track (and velocity) in C2 is similar to the tracks (and velocities) of the low inclination SOHO comets C/1999 R1 and C/2002 R5.
Derek Hammer had left in 2003 August and so there was nobody to measure the positions of the new comet. I derived a prelininary orbit from my own measurements and sent it to Brian Marsden. The orbit was similar to the orbits of C/1999 R1 and C/2002 R5. In 2003 December Karl Battams began measuring and reporting the SOHO comets to CBAT. Karl had a lot of comets to catch up on and measured Kazimieras comet 2004 April 30. The comet was designated C/2003 R5 (MPEC 2004-J59) May 13. Brian Marsden wrote:
R. Kracht remarked already last September on the similarity of the motion of what is now called C/2003 R5 to the motions of his proposed pair C/1999 R1 and C/2002 R5 (see MPEC 2002-S35), fortuitously observed at the same time of the year. The above orbit is essentially identical with that of C/1999 R1 on MPEC 1999-R19.
On 2004 May 17 the new group was announced by Daniel Green (IAUC 8340):
C/2003 R5 belongs to a new group that certainly includes C/1999 R1 and probably includes C/2002 R5.
Orbital elements of the second Kracht group comets compared with those of the other new groups (2004 July):
|C/1999 R1||1999 Sep 05.52||0.0565||43.74||5.22||13.69||48.1||9.4|
|C/2002 R5||2002 Sep 5.79||0.0472||45.38||13.40||14.06||57.9||10.0|
|C/2003 R5||2003 Sep 8.81||0.0569||43.55||5.05||13.59||47.8||9.3|
The weights are the lengths of the observation times (last obs - first obs).
Sebastian Hönig has sucessfully linked C/1999 R1 =
C/2003 R5 (Identification
of a new short-period comet near the sun).
He predicts the next return for about 2007 September 11.
Integrating his orbit backwards with Solex 9.1, I have found these approximate perihelion dates:
1995 September 04 (before SOHO and after SMM)
1991 August 28 (before SOHO and after SMM)
1987 August 19 (SMM images available)
Unfortunately the path of this comet is outside the SOHO LASCO C2 field in mid-August.The C2 FOV is about 3.5 x 3.5 degrees.The SMM FOV is about 3.0 x 3.0 degrees (four quadrants around the sun, each measuring 1.5 x 1.5 degrees).
The returns of C/1999 R1 = C/2003 R5
Bo Zhou found the returning comet in LASCO C2 images of 2007 September 10 19:31 - 21:30 UTC moving very close to the prediction of Sebastian Hönig. Later, I found it entering the C2 field at 2007 September 10 06:54 with an approximate magnitude of mag 9. It was visible in C3 until about 2007 Sep 11 06:18 UTC. It reached mag 5.5 shortly after perihelion in C3. I could not find it in STEREO SECCHI COR2A images close to peak brightness though they showed stars to mag 10. This is a strong argument for the cometary nature of this object.
|P/1999 R1||1999 Sep 05.52||0.0564||43.34||5.39||13.68||47.9||9.3|
|P/2003 R5||2003 Sep 8.82||0.0569||43.62||5.09||13.60||47.9||9.3|
|P/2007 R5||2007 Sep 11.32||0.0537||48.57||0.05||12.64||47.9||9.4|
|P/2011||2011 Sep 07.10||0.0532||48.55||0.08||12.65||47.9||9.4|
Elements from MPEC 2007-S16, Integration to 2011 with Solex.
The orbital elements (peri, node, incl) changed quite a bit
between 2003 and 2007. This is due to a moderately close approach
(<1.4 AU) to Jupiter in May/June 2006.
The comet was observed to be a bit brighter (mag 5.5 instead of mag 6) than at his previously observed two returns.
It will be interesting to see the evolution of this comet.
Will it show fragments? Unfortunately, there is only one
instrument at this time to show the comet: SOHO LASCO shows the
comet close to its perihelion times. It could be lost, if SOHO
LASCO will not be operating 2011 September 06/07.
Perhaps Earth based instruments can image the comet, but it will be quite faint at the larger solar elongations.
The perihelion dates have not much changed with the
new orbit from MPEC 2007-S16:
1995 September 03
1991 August 26
1987 August 17
1983 August 08
Bo Zhou also found the returning comet in LASCO C2 images of 2011 September 06 13:25 - 13:48 UTC. Later that day Michal Kusiak detected the comet in LASCO C3 images from 20:30 and 20:42 UTC. On September 09 the comet was also detected in STEREO SECCHI HI1A and HI1B images by Alan Watson. Man-To Hui measured the HI1A positions the same day and wrote: "Astrometrica seems not good at finding the optcenter of a faint object even when being forced to do such work.". I had measured the C3 positions of September 06 20:18 - 22:30 UTC and could link them with the observations from 1999. 2003 and 2007. When I added Man-To's HI1A positions they showed a strong trend in the residuals, so I could not include them into the solution. From the C2 and C3 observations 1999 - 2011 I got these orbital elements (integration to 2015 with Solex):
|P/1999 R1||1999 Sep 05.52||0.0565||43.36||5.30||13.74||47.8||9.4|
|P/2003 R5||2003 Sep 08.82||0.0571||43.64||5.00||13.66||47.8||9.4|
|P/2007 R5||2007 Sep 11.32||0.0539||48.57||359.96||12.69||47.8||9.5|
|P/2011 R||2011 Sep 07.12||0.0533||48.56||359.99||12.70||47.8||9.5|
|P/2015 R||2015 Sep 04.07||0.0538||48.97||359.57||12.62||47.8||9.5|
A very similar prediction for 2015 is at NK 2328.
P/1999 R1 = 2003 R5 = 2007 R5 has returned in 2011 (P/2011 R4) and in 2015, it had been numbered as 322P/SOHO in June 2015.
The return of C/2002 R5 = C/2008 L6 and L7
2008 June 10 I found a comet in LASCO C2 which moved on the track of C/2002 R5. It was accompanied by a small leading fragment. I could link the observations of the new comet with those of C/2002 R5. The orbital period is 5.8 years, similar the orbital periods of the Kracht and Marsden group comets.
2008 July 24 Brian Marsden issued MPEC 2008-O23,
in which he wrote:
Comets C/2008 L6 and L7 appear to be members of the "Kracht 2" Group, and
R. Kracht suggests that they represent a return of comet C/2002 R5 (cf. MPEC
2002-S35). The 15-deg shift in the line of nodes actually supports the
likely correctness of this linkage, as it is consistent with the comet's
passage within 1.1 AU of Jupiter in Jan. 2007.
Z. Sekanina derived the time of breakup of C/2002 R5 into its fragments C/2008 L6 and C/2008 L7 as most probably between 2 and 10 weeks before the 2002 perihelion and gave an elliptical solution for C/2008 L7 (IAUC 8983, 2008 September 28). The perihelion times of L6 and L7 differ by 18 minutes.
|C/2002 R5||2002 Sep 05.79||0.0472||45.76||13.34||14.17||58.2||10.1|
|C/2008 L6||2008 Jun 10.18||0.0460||58.90||359.83||12.15||58.2||10.4|
|C/2008 L7||2008 Jun 10.17||0.0460||58.93||359.80||12.15||58.2||10.4|
The previous perihelion of C/2002 R5 = 2008 L6 was 1996 November 25.3. The apparent path crosses the C2 field from about November 25.1 - 25.6, but the comet was not found in these images.
NK 2164 predicted the next perihelion of C/2008 L6 for 2014 March 14.98. Zhijian Xu found the comet already 2014 March 07 in LASCO C2 images 04:17 - 05:00 UTC, seven days earlier than expected. The small, leading fragment from 2008 was now trailing by 2.6 hours. The new observations could be linked with those of 2002 and 2008 with A2 = -0.1012 (L6) and A2 = -0.0973 (L7). Orbital elements for C/2002 R5 = 2008 L6 = 2014-ahead:
|C/1996||1996 Nov 18.15||0.0480||45.47||13.61||13.74||3.23294||0.98516||5.813||58.2||9.7|
|C/2002 R5||2002 Sep 05.79||0.0473||45.73||13.31||14.14||3.22416||0.98532||5.789||58.2||10.1|
|C/2008 L6||2008 Jun 10.18||0.0461||58.93||359.73||12.12||3.21235||0.98565||5.758||58.1||10.4|
|C/2014 a||2014 Mar 07.64||0.0452||59.36||359.28||12.07||3.20176||0.98589||5.729||58.1||10.4|
|C/2019||2019 Nov 20.82||0.0433||69.68||348.86||11.28||3.18475||0.98640||5.684||58.2||10.6|
This solution has close approaches to Jupiter with 1.078 au on 2007 January 07 and with 1.251 au on 2018 September 29.
The search for the apparition of 1996 November is difficult (now shifted from November 25 to November 18). Usually there is only one image per hour and the comet is moving with about 80 pixels/h in LASCO C2. And for November 21, 22, 23, 24 there are only 4, 2, 0, 8 C2 images per day. A new search in images from November 17 to December 02 found nothing. The comet may have been too faint to detect with LASCO C2 before it split in 2002 or it passed through the field November 21-24, when there were too few images to detect it.
Orbital evolution of P/2007 R5 and C/2008 L6
Light curves of the "Kracht2 group" comets
Update 2019 June 20
I have asked Zdenek Sekanina if it is possible that the leading component in 2008 could be the trailing component in 2014 and vice versa. He answered that this is possible under some conditions at fragmentation, but wanted me to do the orbital computations again without using the (inferior) C3 observations. My result of these computations show that the leading component in 2008 was the leading component in 2014. So the components did not change places, but the brighter, trailing component in 2008 (C/2008 L6) was the darker, trailing component in 2014.
This result is confirmed by Karl Battam's more extensive measurements of the fragments from 2014, which I have received in 2019 June. Using all available C2 and C3 observations and weighting them according to pixel size (12" and 55") I finally got these results:
Orbital elements for C/2002 R5 = 2008 L6 = 2014-behind (SOHO-2712) with A2 = -1.005*10-9:
|C/1996||1996 Nov 18.204||0.0480||45.53||13.51||14.19||3.23309||0.98516||5.813||58.14||10.08|
|C/2002 R5||2002 Sep 05.794||0.0473||45.79||13.20||14.14||3.22411||0.98532||5.789||58.11||10.08|
|C/2008 L6||2008 Jun 10.181||0.0461||59.01||359.62||12.11||3.21242||0.98565||5.758||58.05||10.36|
|C/2014 behind||2014 Mar 07.744||0.0452||59.43||359.16||12.07||3.20203||0.98588||5.730||58.03||10.37|
|C/2019||2019 Nov 21.080||0.0434||69.81||348.68||11.28||3.18261||0.98638||5.678||58.13||10.58|
This solution has close approaches to Jupiter with 1.079 au on 2007 January 07 and with 1.249 au on 2018 September 29.
According to this solution the darker, leading component in 2008 (C/2008 L7) was the brighter, leading component in 2014. Orbital elements for C/2002 R5 = 2008 L7 = 2014-ahead (SOHO-2673) with A2 = -9.495*10-10:
|C/1996||1996 Nov 18.693||0.0479||46.16||13.33||14.18||3.23364||0.98517||5.815||58.30||10.17|
|C/2002 R5||2002 Sep 05.800||0.0473||46.43||13.02||14.12||3.22366||0.98533||5.788||58.57||10.18|
|C/2008 L7||2008 Jun 10.172||0.0460||59.53||359.55||12.16||3.21206||0.98567||5.757||58.51||10.46|
|C/2014 ahead||2014 Mar 07.642||0.0451||59.96||359.10||12.11||3.20185||0.98591||5.729||58.50||10.47|
|C/2019||2019 Nov 21.337||0.0433||69.98||348.98||11.36||3.18445||0.98641||5.683||58.59||10.67|
This solution has close approaches to Jupiter with 1.085 au on 2007 January 12 and with 1.268 au on 2018 October 03.
This solution for C/2002 R5 = 2008 L7 = SOHO-2673 shows distinct systematic trends in the residuals of 2014. The same is true for C/2002 R5 = 2008 L6 = SOHO-2673 with reversed trends in 2014.
SOHO-2712 can also be linked with C/2002 R5 = 2008 L7 with T = 2019 December 29.14.