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Comet Hyakutake

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This article is about the "Great Comet of 1996". For the 1995 comet of the same name, see C/1995 Y1 (Hyakutake).
C/1996 B2 (Hyakutake)
Comet Hyakutake photographed by Franz Haar in March 1996
Discovery[1]
Discovered byYuji Hyakutake
Discovery siteJapan
Discovery date31 January 1996
Designations
PronunciationJapanese pronunciation: [çakɯ̥take]
Great Comet of 1996
Orbital characteristics[2][3][4]
Epoch15 March 1996 (JD 2450157.5)
Aphelion~1,320 AU (inbound)[a]
~3,500 AU (outbound)
Perihelion0.230 AU
Semi-major axis1,700 AU (outbound)[a]
Eccentricity0.99989
Orbital period~17,000 years (inbound)[a]
~72,000 years (outbound)
Inclination124.922°
188.045°
Argument of
periapsis		130.175°
Last perihelion1 May 1996
TJupiter–0.338
Earth MOID0.101 AU
Jupiter MOID1.991 AU
Physical characteristics[4]
Dimensions4.2 km (2.6 mi)
6 hours
Comet total
magnitude (M1)		7.4
Comet nuclear
magnitude (M2)		11.1
0.0
(1996 apparition)

Comet Hyakutake (formally designated C/1996 B2) is a comet discovered on 31 January 1996.[1] It was dubbed the Great Comet of 1996; its passage to within 0.1 AU (15 Gm) of the Earth on 25 March was one of the closest cometary approaches of the previous 200 years. Reaching an apparent visual magnitude of zero and spanning nearly 80°, Hyakutake appeared very bright in the night sky and was widely seen around the world. The comet temporarily upstaged the much anticipated Comet Hale–Bopp, which was approaching the inner Solar System at the time.

Hyakutake is a long-period comet that passed perihelion on 1 May 1996. Before its most recent passage through the Solar System, its orbital period was about 17,000 years,[2][5] but the gravitational perturbation of the giant planets has increased this period to 70,000 years.[2][5] This is the first comet to have an X-ray emission detected, which is most likely the result of ionised solar wind particles interacting with neutral atoms in the coma of the comet. The Ulysses spacecraft fortuitously crossed the comet's tail at a distance of more than 500 million km (3.3 AU; 310 million mi) from the nucleus, showing that Hyakutake had the longest tail known for a comet.

Discovery

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The comet was discovered on 30 January 1996,[1] by Yuji Hyakutake, an amateur astronomer from southern Japan.[6] He had been searching for comets for years and had moved to Kagoshima Prefecture partly for the dark skies in nearby rural areas. He was using a powerful set of binoculars with 150 mm (6 in) objective lenses to scan the skies on the night of the discovery.[7]

This comet was actually the second Comet Hyakutake; Hyakutake had discovered comet C/1995 Y1 several weeks earlier.[8] While re-observing his first comet (which never became visible to the naked eye) and the surrounding patch of sky, Hyakutake was surprised to find another comet in almost the same position as the first had been. Hardly believing a second discovery so soon after the first, Hyakutake reported his observation to the National Astronomical Observatory of Japan the following morning.[9] Later that day, the discovery was confirmed by independent observations.[10]

At the time of its discovery, the comet was shining at magnitude 11.0 and had a coma approximately 2.5 arcminutes across. It was approximately 2 astronomical units (AU) from the Sun.[11] Later, a precovery image of the comet was found on a photograph taken on January 1, when the comet was about 2.4 AU from the Sun and had a magnitude of 13.3.[5]

Orbit

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Comet Hyakutake's trajectory through the inner solar system, with a high inclination, passed closest to the earth in late March 1996, passing over the earth's north pole. It was at perihelion on May 1.

When the first calculations of the comet's orbit were made, scientists realized that it was going to pass just 0.1 AU from Earth on 25 March.[12] Only four comets in the previous century had passed closer.[13] Comet Hale–Bopp was already being discussed as a possible "great comet"; the astronomical community eventually realised that Hyakutake might also become spectacular because of its close approach.[14]

Moreover, Comet Hyakutake's orbit meant that it had last been to the inner Solar System approximately 17,000 years earlier.[2] Because it had probably passed close to the Sun several times before,[5] the approach in 1996 would not be a maiden arrival from the Oort cloud, a place from where comets with orbital periods of millions of years come. Comets entering the inner Solar System for the first time may brighten rapidly before fading as they near the Sun, because a layer of highly volatile material evaporates. This was the case with Comet Kohoutek in 1973; it was initially touted as potentially spectacular, but only appeared moderately bright. Older comets show a more consistent brightening pattern.[15] Thus, all indications suggested Comet Hyakutake would be bright.[14]

Besides approaching close to Earth, the comet would also be visible throughout the night to northern hemisphere observers at its closest approach because of its path, passing very close to the pole star. This would be an unusual occurrence, because most comets are close to the Sun in the sky when the comets are at their brightest, leading to the comets appearing in a sky not completely dark.[16]

Earth passage

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The path of Comet Hyakutake across the sky

Hyakutake became visible to the naked eye in early March 1996. By mid-March, the comet was still fairly unremarkable, shining at 4th magnitude with a tail about 5 degrees long. As it neared its closest approach to Earth, it rapidly became brighter, and its tail grew in length. By March 24, the comet was one of the brightest objects in the night sky, and its tail stretched 35 degrees. The comet had a notably bluish-green colour.[5]

The comet on the evening of its closest approach to Earth on 25 March 1996

The closest approach occurred on 25 March at a distance of 0.1 AU (15 million km; 39 LD).[4] Hyakutake was moving so rapidly across the night sky that its movement could be detected against the stars in just a few minutes; it covered the diameter of a full moon (half a degree) every 30 minutes. Observers estimated its magnitude as around 0, and tail lengths of up to 80 degrees were reported.[5] Its coma, now close to the zenith for observers at mid-northern latitudes, appeared approximately 1.5 to 2 degrees across, roughly four times the diameter of the full moon.[5] The comet's head appeared distinctly blue-green, possibly due to emissions from diatomic carbon (C2) combined with sunlight reflected from dust grains.[17]

Because Hyakutake was at its brightest for only a few days, it did not have time to permeate the public imagination in the way that Comet Hale–Bopp did the following year. Many European observers in particular did not see the comet at its peak because of unfavourable weather conditions.[5]

Perihelion and afterwards

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After its close approach to the Earth, the comet faded to about 2nd magnitude. It reached perihelion on 1 May 1996, brightening again and exhibiting a dust tail in addition to the gas tail seen as it passed the Earth. By this time, however, it was close to the Sun and was not seen as easily. It was observed passing perihelion by the SOHO Sun-observing satellite, which also recorded a large coronal mass ejection being formed at the same time. The comet's distance from the Sun at perihelion was 0.23 AU, well inside the orbit of Mercury.[13]

After its perihelion passage, Hyakutake faded rapidly and was lost to naked-eye visibility by the end of May. Its orbital path carried it rapidly into the southern skies, but following perihelion it became much less monitored. The last known observation of the comet took place on November 2.[18]

Hyakutake had passed through the inner Solar System approximately 17,000 years ago; gravitational interactions with the gas giants during its 1996 passage stretched its orbit greatly, and barycentric fits to the comet's orbit predict it will not return to the inner Solar System again for approximately 70,000 years.[2][5][a]

Scientific results

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Spacecraft passes through the tail

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Animation of Ulysses' trajectory from 6 October 1990 to 29 June 2009
  Ulysses ·   Earth ·   Jupiter ·   C/2006 P1 ·   C/1996 B2 ·   C/1999 T1

The Ulysses spacecraft made an unexpected pass through the tail of the comet on 1 May 1996.[19] Evidence of the encounter was not noticed until 1998. Astronomers analysing old data found that Ulysses' instruments had detected a large drop in the number of protons passing, as well as a change in the direction and strength of the local magnetic field. This implied that the spacecraft had crossed the 'wake' of an object, most likely a comet; the object responsible was not immediately identified.[20]

In 2000, two teams independently analyzed the same event. The magnetometer team realized that the changes in the direction of the magnetic field mentioned above agreed with the "draping" pattern expected in a comet's ion, or plasma tail. The magnetometer team looked for likely suspects. No known comets were located near the satellite, but looking further afield, they found that Hyakutake, 500 million km (3.3 AU) away, had crossed Ulysses' orbital plane on 23 April 1996. The solar wind had a velocity at the time of about 750 km/s (470 mi/s), at which speed it would have taken eight days for the tail to be carried out to where the spacecraft was situated at 3.73 AU, approximately 45 degrees out of the ecliptic plane. The orientation of the ion tail inferred from the magnetic field measurements agreed with the source lying in Comet Hyakutake's orbital plane.[21]

The other team, working on data from the spacecraft's ion composition spectrometer, discovered a sudden large spike in detected levels of ionised particles at the same time. The relative abundances of chemical elements detected indicated that the object responsible was definitely a comet.[22]

Based on the Ulysses encounter, the comet's tail is known to have been at least 570 million km (360 million miles; 3.8 AU) long. This is almost twice as long as the previous longest-known cometary tail, that of the Great Comet of 1843, which was 2 AU long.[21] This record was broken in 2002 by comet 153P/Ikeya–Zhang, which had a tail-length of at least 7.46 AU.[23]

Composition

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Terrestrial observers found ethane and methane in the comet, the first time either of these gases had been detected in a comet. Chemical analysis showed that the abundances of ethane and methane were roughly equal, which may imply that its ices formed in interstellar space, away from the Sun, which would have evaporated these volatile molecules. Hyakutake's ices must have formed at temperatures of 20 K or less, indicating that it probably formed in a denser-than-average interstellar cloud.[24]

The amount of deuterium in the comet's water ices was determined through spectroscopic observations. It was found that the ratio of deuterium to hydrogen (known as the D/H ratio) was about 3×10−4, which compares to a value in Earth's oceans of about 1.5×10−4. It has been proposed that cometary collisions with Earth might have supplied a large proportion of the water in the oceans, but the high D–H ratio measured in Hyakutake and other comets such as Hale–Bopp and Halley's Comet have caused problems for this theory.[25]

X-ray emission

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X-ray emission from Hyakutake, as seen by the ROSAT satellite

One of the great surprises of Hyakutake's passage through the inner Solar System was the discovery that it was emitting X-rays, with observations made using the ROSAT satellite revealing very strong X-ray emission.[26] This was the first time a comet had been seen to do so, but astronomers soon found that almost every comet they looked at was emitting X-rays. The emission from Hyakutake was brightest in a crescent shape surrounding the nucleus with the ends of the crescent pointing away from the Sun.[27]

The cause of the X-ray emission is thought to be a combination of two mechanisms. Interactions between energetic solar wind particles and cometary material evaporating from the nucleus is likely to contribute significantly to this effect.[28] Reflection of solar X-rays is seen in other Solar System objects such as the Moon, but a simple calculation assuming even the highest X-ray reflectivity possible per molecule or dust grain is not able to explain the majority of the observed flux from Hyakutake, as the comet's atmosphere is very tenuous and diffuse. Observations of comet C/1999 S4 (LINEAR) with the Chandra satellite in 2000 determined that X-rays observed from that comet were produced predominantly by charge exchange collisions between highly charged carbon, oxygen and nitrogen minor ions in the solar wind, and neutral water, oxygen and hydrogen in the comet's coma.[29]

Nucleus size and activity

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Comet Hyakutake captured by the Hubble Space Telescope on 4 April 1996, with an infrared filter
The region around the nucleus of Comet Hyakutake, as seen by the Hubble Space Telescope. Some fragments can be seen breaking off.

Radar results from the Arecibo Observatory indicated that the comet nucleus was about 4.8 km (3 mi) across, and surrounded by a flurry of pebble-sized particles ejected at a few metres per second. This size measurement corresponded well with indirect estimates using infrared emission and radio observations.[30][31]

The small size of the nucleus (Halley's Comet is about 15 km (9.3 mi) across, while Comet Hale–Bopp was about 60 km (37 mi) across) implies that Hyakutake must have been very active to become as bright as it did. Most comets undergo outgassing from a small proportion of their surface, but most or all of Hyakutake's surface seemed to have been active. The dust production rate was estimated to be about 2×103 kg/s at the beginning of March, rising to 3×104 kg/s as the comet approached perihelion. During the same period, dust ejection velocities increased from 50 m/s to 500 m/s.[32][33]

Observations of material being ejected from the nucleus allowed astronomers to establish its rotation period. As the comet passed the Earth, a large puff or blob of material was observed being ejected in the sunward direction every 6.23 hours. A second smaller ejection with the same period confirmed this as the rotation period of the nucleus.[34]

See also

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Notes

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  1. ^ Solution using the Solar System Barycenter. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates.

References

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  2. ^ a b c d e Horizons output (30 January 2011). "Barycentric Osculating Orbital Elements for Comet Hyakutake (C/1996 B2)". Archived from the original on 5 June 2019. Retrieved 31 January 2011.
  3. ^ "Comet Hyakutake: Orbital elements and 10-day ephemeris". European Southern Observatory. Archived from the original on 3 February 2009.
  4. ^ a b c "C/1996 B2 (Hyakutake) – JPL Small-Body Database Lookup". ssd.jpl.nasa.gov. Jet Propulsion Laboratory. Retrieved 24 December 2024.
  5. ^ a b c d e f g h i N. D. James (1998). "Comet C/1996 B2 (Hyakutake): The Great Comet of 1996". Journal of the British Astronomical Association. 108: 157–171. Bibcode:1998JBAA..108..157J.
  6. ^ R. Baalke (24 March 1996). "Comet C/1996 B2 Hyakutake". NASA / JPL. Archived from the original on 6 January 2011. Retrieved 9 January 2007.
  7. ^ E. L. Aguirre. "How Yuji Hyakutake Found His Comet". Sky & Telescope. Archived from the original on 3 February 2009. Retrieved 21 April 2008.
  8. ^ G. Tenmon; Y. Hyakutake (April 1996). "How Comet Hyakutake B2 Was Discovered" (in Japanese). Translated by M. Okamoto. NASA. Archived from the original on 12 June 2011. Retrieved 9 January 2007.
  9. ^ Y. Hyakutake (29 March 1996). "Press Statement by Mr. Yuji Hyakutake Discoverer of Comet Hyakutake" (Press release). Archived from the original on 21 February 2012. Retrieved 13 February 2007.
  10. ^ B. G. Marsden (3 February 1996). "Comet C/1996 B2 (Hyakutake)". Central Bureau for Astronomical Telegrams. 6303. Bibcode:1996IAUC.6303....1G.
  11. ^ "Press Information Sheet: Comet C/1996 B2 (Hyakutake)" (Press release). Harvard-Smithsonian Center for Astrophysics. 20 November 1996. Archived from the original on 21 November 2007. Retrieved 16 October 2007.
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  18. ^ "Nakano Note 838". Archived from the original on 24 July 2011. Retrieved 12 May 2008.
  19. ^ "Comet Hyakutake makes a mark on Ulysses". PhysicsWorld. 6 April 2000. Archived from the original on 9 November 2020. Retrieved 10 November 2020.
  20. ^ G. H. Jones (29 July – 2 August 2002). B. Warmbein (ed.). Ulysses's encounters with comet Hyakutake. Proceedings of Asteroids, Comets, Meteors - ACM 2002. International Conference. Berlin, Germany: ESA Publications Division. pp. 563–566. Bibcode:2002ESASP.500..563J. ISBN 92-9092-810-7.
  21. ^ a b G. H. Jones; A. Balogh; T. S. Horbury (2000). "Identification of comet Hyakutake's extremely long ion tail from magnetic field signatures". Nature. 404 (6778): 574–576. Bibcode:2000Natur.404..574J. doi:10.1038/35007011. PMID 10766233. S2CID 4418311.
  22. ^ G. Gloeckler; J. Geiss; N. A. Schwadron; L. A. Fisk; T. H. Zurbuchen; et al. (2000). "Interception of comet Hyakutake's ion tail at a distance of 500 million kilometres" (PDF). Nature. 404 (6778): 576–578. Bibcode:2000Natur.404..576G. doi:10.1038/35007015. hdl:2027.42/62756. PMID 10766234. S2CID 4420901.
  23. ^ G. H. Jones; H. A. Elliott; D. J. McComas; M. E. Hill; et al. (2020). "Cometary ions detected by the Cassini spacecraft 6.5 au downstream of Comet 153P/Ikeya-Zhang". arXiv:2006.00500 [astro-ph.EP].
  24. ^ M. J. Mumma; M. A. Disanti; N. dello Russo; M. Fomenkova; et al. (1996). "Detection of Abundant Ethane and Methane, Along with Carbon Monoxide and Water, in Comet C/1996 B2 Hyakutake: Evidence for Interstellar Origin". Science. 272 (5266): 1310–1314. Bibcode:1996Sci...272.1310M. doi:10.1126/science.272.5266.1310. PMID 8650540. S2CID 27362518.
  25. ^ D. Bockelée-Morvan; D. Gautier; D. C. Lis; K. Young; J. Keene; et al. (1998). "Deuterated Water in Comet C/1996 B2 (Hyakutake) and Its Implications for the Origin of Comets" (PDF). Icarus. 133 (1): 147–162. Bibcode:1998Icar..133..147B. doi:10.1006/icar.1998.5916. hdl:2060/19980035143. S2CID 121830932.
  26. ^ J. Glanz (1996). "Comet Hyakutake Blazes in X-rays". Science. 272 (5259): 194. Bibcode:1996Sci...272..194G. doi:10.1126/science.272.5259.194. S2CID 120173459.
  27. ^ T. E. Cravens (2002). "X-ray Emission from Comets". Science. 296 (5570): 1042–1046. Bibcode:2002Sci...296.1042C. doi:10.1126/science.1070001. PMID 12004110. S2CID 26407069.
  28. ^ C. M. Lisse; K. Dennerl; J. Englhauser; M. Harden; F. E. Marshall; et al. (1996). "Discovery of X-ray and Extreme Ultraviolet Emission from Comet C/Hyakutake 1996 B2" (PDF). Science. 274 (5285): 205–209. Bibcode:1996Sci...274..205L. doi:10.1126/science.274.5285.205. S2CID 122700701.
  29. ^ C. M. Lisse; D. J. Christian; K. Dennerl; K. J. Meech; et al. (2001). "Charge Exchange-Induced X-Ray Emission from Comet C/1999 S4 (LINEAR)". Science. 292 (5520): 1343–1348. Bibcode:2001Sci...292.1343L. doi:10.1126/science.292.5520.1343. PMID 11359004.
  30. ^ J. Sarmecanic; M. Fomenkova; B. Jones; T. Lavezzi (1997). "Constraints on the Nucleus and Dust Properties from Mid-Infrared Imaging of Comet Hyakutake". Astrophysical Journal Letters. 483 (1): L69 – L72. Bibcode:1997ApJ...483L..69S. doi:10.1086/310726. PMID 11541247. S2CID 24944390.
  31. ^ C. M. Lisse; Y. R. Fernández; A. Kundu; M. F. A'Hearn; A. Dayal; et al. (1999). "The Nucleus of Comet Hyakutake (C/1996 B2)". Icarus. 140 (1): 189–204. Bibcode:1999Icar..140..189L. doi:10.1006/icar.1999.6131.
  32. ^ M. Fulle; H. Mikuz; S. Bosio (1997). "Dust environment of Comet Hyakutake 1996 B2". Astronomy and Astrophysics. 324: 1197–1205. Bibcode:1997A&A...324.1197F.
  33. ^ D. C. Jewitt; H. E. Matthews (1997). "Submillimeter Continuum Observations of Comet Hyakutake (1996 B2)". Astronomical Journal. 113: 1145. Bibcode:1997AJ....113.1145J. doi:10.1086/118333.
  34. ^ D. G. Schleicher; R. L. Millis; D. J. Osip; S. M. Lederer (1998). "Activity and the Rotation Period of Comet Hyakutake (1996 B2)". Icarus. 131 (2): 233–244. Bibcode:1998Icar..131..233S. doi:10.1006/icar.1997.5881.

Further reading

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