| 96P/Machholz | |
| Discoverer: | Donald Machholz |
| Discovery Date: | May 12, 1986 |
| Designations: | 96P, Machholz, Machholz 1, 1986 J2, 1991 XII, 1986e, 1986 VII |
| Epoch: | 2028-May-29 (JD 2461920.5) |
| Semimajor: | 3.030 AU |
| Perihelion: | 0.1160 AU (38% of Mercury's perihelion) |
| Aphelion: | 5.944 AU |
| Eccentricity: | 0.9617 |
| Period: | 5.27 yr |
| Inclination: | 57.49° |
| Max Speed: | 122km/s |
| Last P: | January 31, 2023, 02:02 UTC October 27, 2017, 23:03 UTC |
| Next P: | ≈May 12, 2028 |
Comet 96P/Machholz or 96P/Machholz 1 is a short-period sungrazing comet discovered on May 12, 1986, by amateur astronomer Donald Machholz on Loma Prieta peak, in central California using 130mm binoculars. On June 6, 1986, 96P/Machholz passed 0.404abbr=onNaNabbr=on from the Earth. 96P/Machholz last came to perihelion on January 31, 2023. The comet has an estimated diameter of around 6.4km (04miles).
96P/Machholz is unusual among comets in several respects. Other than small SOHO comets, its highly eccentric 5.29 year orbit has the smallest perihelion distance known among numbered/regular short-period comets, bringing it considerably closer to the Sun than the orbit of Mercury. It is also the only known short-period comet with both high orbital inclination and high eccentricity. In 2007, 96P/Machholz was found to be both carbon-depleted and cyanogen-depleted, a chemical composition nearly unique among comets with known compositions. The chemical composition implies a different and possible extrasolar origin.[1]
The orbit of 96P/Machholz corresponds to the Arietids and the Marsden and Kracht comet groups. Its Tisserand parameter with respect to Jupiter, TJ, is 1.94 and comets are generally classified as Jupiter family if TJ > 2. Orbital integrations indicate that TJ was greater than 2 about 2500 years ago. 96P/Machholz is currently in a 9:4 orbital resonance with Jupiter. It will not make another close approach to the Earth until 2028, when it will pass at a distance of 0.3197abbr=onNaNabbr=on. It may eventually be ejected from the Solar System.[2]
| 2139-Jun-13 23:28 ± 13 hours | 0.179abbr=unitNaNabbr=unit | 1.06AU | 41.4 | 37.1 | ± 500 thousand km | Horizons |
| Perihelion distance at different epochs | |||||||
| Perihelion (AU) | |||||||
|---|---|---|---|---|---|---|---|
| 1897 | 0.169 | ||||||
| 1928 | 0.152 | ||||||
| 1939 | 0.145 | ||||||
| 1975 | 0.133 | ||||||
| 1986 | 0.127 | ||||||
| 2023 | 0.116 | ||||||
| 2038 | 0.109 | ||||||
| 2081 | 0.095 | ||||||
| 2102 | 0.093 | ||||||
Machholz 1 entered the field of view of the orbiting Solar and Heliospheric Observatory (SOHO) in 1996, 2002, 2007, 2012, and 2017, where it was seen by the corona-observing LASCO instrument in its C2 and C3 coronagraphs.
During the 2001/2002 passage the comet brightened to magnitude −2, and was very impressive as seen by SOHO.
In 2007, it appeared in SOHO's LASCO C3's field of view from April 2 to 6, peaking in brightness on April 4, 2007, around magnitude +2. In these observations, its coma was substantially smaller than the Sun in volume, but the forward scattering of light made the comet appear significantly brighter.
The comet SOHO 2333 is believed to be a fragment of Machholz that came off during the 2007 perihelion. It was discovered by Indian amateur astronomer Prafull Sharma in August 2012 by analyzing data from the Solar and Heliospheric Observatory, specifically the Large Angle and Spectrometric Coronagraph.[3] Data analysis of this sort has become commonplace based on public availability of SOHO images. Sharma became the third Indian to have discovered a comet in this manner.[4]
Between July 12–17, 2012, 96P/Machholz was visible in the SOHO LASCO/C3 field of view and expected to brighten to about magnitude +2. Two small faint fragments of 96P/Machholz were detected in the SOHO C2 images. The fragments were five hours ahead of 96P/Machholz, and probably fragmented from the comet during the 2007 perihelion passage.
The 2017 perihelion was on October 27, 2017. At closest approach, it passed 0.12395abbr=onNaNabbr=on from the Sun. Coronagraphs on SOHO were monitoring the flyby for a fifth time. Its peak brightness was expected to be about 2.0, when it was closest to the Sun.[5]
The January 31, 2023 perihelion passage was the sixth passage observed by SOHO.[6] On February 4, 2023, the comet was recovered in the morning sky 2 degrees above the horizon at around magnitude 7.[7]
Using observations through October 2022, which is three months before the 2023 perihelion passage, the comet will next come to perihelion around May 12, 2028.
Spectrographic analysis of the coma of 96P/Machholz was made during its 2007 apparition, as part of the Lowell Observatory comet composition long-term observing program. When compared with the measured abundances of five molecular species in the comae of the other 150 comets in their database, these measurements showed 96P/Machholz to have far fewer carbon molecules. These other comets had on average 72 times as much cyanogen as 96P/Machholz.
The only comet previously seen with similar depletion both in carbon-chain molecules and cyanogens is, but it has a substantially different orbit.
There are currently three hypotheses to explain the chemical composition of 96P/Machholz. One hypothesis for the difference is that 96P/Machholz was an interstellar comet from outside the Solar System and was captured by the Sun. Other possibilities are that it formed in an extremely cold region of the Solar System (such that most carbon gets trapped in other molecules). Given how close it approaches the Sun at perihelion, repeated baking by the Sun may have stripped most of its cyanogen.
The following table represents future orbital elements for 96P keeping in mind that results hundreds of years in the future are highly speculative given the uncertain behavior of nongravitational forces over long time intervals and divergent solutions. By the year 2235 the uncertainty in the comets position is more than 1abbr=unitNaNabbr=unit.[8]
| 1600 | 1700 | 1800 | 1900 | 2000 | 2100 | 2200 | 2300 | 2400 | 2500 | ||
| Periapsis (au) | 0.34 | 0.27 | 0.23 | 0.17 | 0.12 | 0.09 | 0.07 | 0.04 | 0.03 | 0.03 | |
| Apoapsis (au) | 5.73 | 5.77 | 5.85 | 5.88 | 5.90 | 5.97 | 6.01 | 6.01 | 6.01 | 6.02 | |
| Inclination (degrees) | 70.87 | 69.65 | 66.35 | 63.62 | 60.11 | 53.20 | 44.00 | 32.36 | 15.08 | 16.82 | |
| Eccentricity | 0.89 | 0.91 | 0.93 | 0.94 | 0.96 | 0.97 | 0.98 | 0.99 | 0.99 | 0.99 |