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Sungrazing comet

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The representative orbit of a sungrazing comet.

Asungrazing cometis acometthat passes extremely close to theSunatperihelion– sometimes within a few thousand kilometres of the Sun's surface. Although small sungrazers can completelyevaporateduring such a close approach to the Sun, larger sungrazers can survive many perihelion passages. However, the strong evaporation andtidal forcesthey experience often lead to their fragmentation.

Up until the 1880s, it was thought that all bright comets near the Sun were the repeated return of a single sungrazing comet. Then, German astronomerHeinrich Kreutzand American astronomerDaniel Kirkwooddetermined that, instead of the return of the same comet, each appearance was a different comet, but each were related to a group of comets that had separated from each other at an earlier passage near the Sun (atperihelion).[1]Very little was known about the population of sungrazing comets until 1979 whencoronagraphicobservations allowed the detection of sungrazers. As of October 21, 2017, there are 1495 known comets that come within ~12 solar radii (~0.055 AU).[2]This accounts for nearly one third of all comets.[3]Most of these objects vaporize during their close approach, but a comet with a nucleus radius larger than 2–3 km is likely to survive the perihelion passage with a final radius of ~1 km.

Sungrazer comets were some of the earliest observed comets because they can appear very bright. Some are even consideredGreat Comets.The close passage of a comet to the Sun will brighten the comet not only because of the reflection off the comet nucleus when it is closer to the Sun, but the Sun also vaporizes a large amount of gas from the comet and the gas reflects more light. This extreme brightening will allow for possible naked eye observations from Earth depending on howvolatilethe gases are and if the comet is large enough to survive perihelion. These comets provide a useful tool for understanding the composition of comets as we observe the outgassing activity and they also offer a way to probe the effects solar radiation has on other Solar System bodies.

History of sungrazers

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Pre-19th century

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One of the first comets to have its orbit computed was the sungrazing comet (and Great Comet) of 1680, now designatedC/1680 V1.It was observed byIsaac Newtonand he published the orbit results in 1687.[4]Later, in 1699,Jacques Cassiniproposed that comets could have relatively short orbital periods and that C/1680 V1 was the same as a comet observed byTycho Brahein 1577, but in 1705Edmond Halleydetermined that the difference between the perihelion distances of the two comets was too great for them to be the same object.[5][6]However, this marked the first time that it was hypothesized that Great Comets were related or perhaps the same comet. Later,Johann Franz Enckecomputed the orbit of C/1680 V1 and found a period of approximately 9000 years, leading him to conclude that Cassini's theory of short period sungrazers was flawed. C/1680 V1 had the smallest measured perihelion distance until the observation in 1826 of comet C/1826 U1.[4]

19th century

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Advances were made in understanding sungrazing comets in the 19th century with the Great Comets of1843,C/1880 C1, and1882.C/1880 C1 and C/1843 D1 had very similar appearances and also resembled theGreat Comet of 1106,therefore Daniel Kirkwood proposed that C/1880 C1 and C/1843 D1 were separate fragments of the same object.[1]He also hypothesized that theparent bodywas a comet seen byAristotleandEphorusin 371 BC because there was a supposed claim that Ephorus witnessed the comet splitting after perihelion.[4]

CometC/1882 R1appeared only two years after the previously observed sungrazer so this convinced astronomers that these bright comets were not all the same object. Some astronomers theorized that the comet might pass through a resisting medium near the Sun and that would shorten its period.[4]When astronomers observed C/1882 R1, they measured the period before and after perihelion and saw no shortening in the period which disproved the theory. After perihelion this object was also seen to split into several fragments and therefore Kirkwood's theory of these comets coming from a parent body seemed like a good explanation.

In an attempt to link the 1843 and 1880 comets to the comet in 1106 and 371 BC, Kreutz measured the fragments of the 1882 comet and determined that it was likely a fragment of the 1106 comet. He then designated that all sungrazing comets with similar orbital characteristics as these few comets would be part of theKreutz Group.[4]

The 19th century also provided the first spectrum taken of a comet near the Sun which was taken by Finlay & Elkin in 1882.[7]Later the spectrum was analyzed andFeandNispectral lines were confirmed.[8]

20th century

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The first sungrazing comet observed in the 20th century was in 1945 and then between 1960 and 1970 five sungrazing comets were seen (C/1961 O1,C/1962 C1,C/1963 R1,C/1965 S1,andC/1970 K1). The 1965 comet (Comet Ikeya-Seki) allowed for measurements of spectral emission lines and several elements were detected including Iron, marking this the first comet since the Great Comet of 1882 to show this feature. Other emission lines includedK,Ca,Ca+,Cr,Co,Mn,Ni,Cu,andV.[9][10][11][12][13]Comet Ikeya-Seki also led to separating the Kreutz sungrazers into two subgroups by Brian Marsden in 1967.[14]One subgroup appears to have the 1106 comet as the parent body and members are fragments of that comet, while the other group have similar dynamics but no confirmed parent body associated with it.

Coronagraphic observations

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The 20th century greatly impacted sungrazing comet research with the launch ofcoronagraphictelescopes includingSolwind,SMM,andSOHO.Until this point, sungrazing comets were only seen with thenaked eyebut with the coronagraphic telescopes many sungrazers were observed that were much smaller and very few have survived perihelion passage. The comets observed by Solwind and SMM from 1981 to 1989 hadvisual magnitudesfrom about -2.5 to +6 which is much fainter than Comet Ikeya-Seki with a visual magnitude of about -10.[4]

In 1987 and 1988 it was first observed by SMM that there could be pairs of sungrazing comets that can appear within very short time periods ranging from a half of a day up to about two weeks. Calculations were made to determine that the pairs were part of the same parent body but broke apart at tens of AU from the Sun.[15]The breakup velocities were only on the order of a few meters per second which is comparable to the speed of rotation for these comets. This led to the conclusion that these comets break fromtidal forcesand that comets C/1882 R1, C/1965 S1, and C/1963 R1 probably broke off from the Great Comet of 1106.[16]

Coronagraphs allowed for measuring the properties of the comet as it reached very close to the Sun. It was noted that sungrazing comets tend to peak in brightness at a distance of about 12.3solar radiior 11.2 solar radii. It is thought that this variation stems from a difference in dust composition. Another small peak in brightness has been found at about 7 solar radii from the sun and it is possibly due to a fragmentation of the comet nucleus.[4]An alternative explanation is that the brightness peak at 12 solar radii comes from the sublimation ofamorphousolivinesand the peak at 11.2 solar radii is from the sublimation ofcrystallineolivines. The peak at 7 solar radii could then be thesublimationofpyroxene.[17]

Sungrazing groups

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Kreutz Sungrazers

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Main article:Kreutz sungrazer

The most famous sungrazers are the Kreutz Sungrazers, which all originate from one giant comet that broke up into many smaller comets during its first passage through the inner Solar System. An extremely bright comet seen byAristotleandEphorusin 371 BC is a possible candidate for this parent comet.

TheGreat Cometsof1843and1882,Comet Ikeya–Sekiin 1965 andC/2011 W3 (Lovejoy)in 2011 were all fragments of the original comet. Each of these four was briefly bright enough to be visible in the daytime sky, next to the Sun, 1882's comet outshining even thefull moon.

In 1979,C/1979 Q1 (SOLWIND)was the first sungrazer to be spotted by US satelliteP78-1,incoronagraphstaken on 30 and 31 Aug 1979.[18]

Apart from Comet Lovejoy, none of the sungrazers seen bySOHOhas survived its perihelion passage; some may have plunged into the Sun itself, but most are likely to have simply evaporated away completely.[19]

Other sungrazers

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Comet ISON[20]taken with the Wide Field Camera 3 on April 30, 2013.[21]

About 83% of the sungrazers observed with SOHO are members of the Kreutz group.[22]The other 17% contains some sporadic sungrazers, but three other related groups of comets have been identified among them: the Kracht, Marsden and Meyer groups. The Marsden and Kracht groups both appear to be related to Comet96P/Machholz.These comets have also been linked to severalmeteorstreams, including the DaytimeArietids,thedelta Aquariids,and theQuadrantids.Linked comet orbits suggest that both Marsden and Kracht groups have a small period, on the order of five years, but the Meyer group may have intermediate- or long-period orbits. The Meyer group comets are typically small, faint, and never have tails. TheGreat Comet of 1680was a sungrazer and while used by Newton to verify Kepler's equations on orbital motion, it was not a member of any larger groups. However, cometC/2012 S1 (ISON),which disintegrated shortly beforeperihelion,[20]had orbital elements similar to the Great Comet of 1680 and could be a second member of the group.[23]

Origin of sungrazing comets

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Studies show that for comets with highorbital inclinationsand perihelion distances of less than about 2astronomical units,the cumulative effect of gravitational perturbations over many orbits is adequate to reduce the perihelion distance to very small values. One study has suggested thatComet Hale–Bopphas about a 15% chance of eventually becoming a sungrazer.

Role in solar astronomy

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The motion of tails of sungrazers that survive perihelion (such as Comet Lovejoy) can provide solar astronomers with information about the structure of thesolar corona,particularly the detailed magnetic structure.[24]

See also

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Footnotes

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  1. ^abKirkwood, Daniel (November 1880). "On the great southern comet of 1880".The Observatory.3:590–592.Bibcode:1880Obs.....3..590K.
  2. ^JPL Small-Body Database Search Engine
  3. ^Johnston, Robert (27 July 2013)."Known populations of solar system objects".Retrieved30 July2013.
  4. ^abcdefgMarsden, Brian G. (September 2005). "Sungrazing Comets".Annual Review of Astronomy & Astrophysics.43(1): 75–102.Bibcode:2005ARA&A..43...75M.doi:10.1146/annurev.astro.43.072103.150554.
  5. ^Cassini, JD (1699).Hist. Acad. R. Sci. Paris.Amsterdam ed. 1734: 95–100.{{cite journal}}:Missing or empty|title=(help)
  6. ^Halley, Edmund (1705)."IV. Astronomiæ cometicæ synopsis, Autore Edmundo Halleio apud Oxonienses Geometriæ Professore Saviliano, & Reg. Soc. S".Phil. Trans.24(297): 1882–1899.Bibcode:1704RSPT...24.1882H.doi:10.1098/rstl.1704.0064.
  7. ^Finlay, W.H.; W.L Elkin (November 1992)."Observations of the Great Comet 1882".Monthly Notices of the Royal Astronomical Society.43:21–25.Bibcode:1882MNRAS..43...22E.doi:10.1093/mnras/43.1.21.
  8. ^Orlov, A. (1927).Astron. Zh.4:1–9.{{cite journal}}:Missing or empty|title=(help)
  9. ^Dufay, J.; Swings, P.; Fehrenbach, Ch. (November 1965)."Spectrographic Observations of Comet Ikeya-Seki (1965f)"(PDF).Astrophysical Journal.142:1698.Bibcode:1965ApJ...142.1698D.doi:10.1086/148467.
  10. ^Curtis, G. Wm.; Staff, The Sacramento Peak Observatory (April 1966)."Daylight observations of the 1965 F comet at the Sacramento Peak Observatory".The Astronomical Journal.71:194.Bibcode:1966AJ.....71..194C.doi:10.1086/109902.
  11. ^Thackeray, A. D.; Feast, M. W.;Warner, B.(January 1966). "Daytime Spectra of Comet Ikeya-Seki Near Perihelion".The Astrophysical Journal.143:276.Bibcode:1966ApJ...143..276T.doi:10.1086/148506.
  12. ^Preston, G. W. (February 1967)."The spectrum of Ikkeya-Seki (1965f)".The Astrophysical Journal.147:718.Bibcode:1967ApJ...147..718P.doi:10.1086/149049.
  13. ^Slaughter, C. D. (September 1969)."The Emission Spectrum of Comet Ikeya-Seki 1965-f at Perihelion Passage".The Astronomical Journal.74:929.Bibcode:1969AJ.....74..929S.doi:10.1086/110884.
  14. ^Marsden, B. G. (November 1967). "The sungrazing comet group".The Astronomical Journal.72:1170.Bibcode:1967AJ.....72.1170M.doi:10.1086/110396.
  15. ^Sekanina, Zdenek (20 October 2000)."Secondary Fragmentation of theSolar and Heliospheric ObservatorySungrazing Comets at Very Large Heliocentric Distance ".The Astrophysical Journal.542(2): L147–L150.Bibcode:2000ApJ...542L.147S.doi:10.1086/312943.S2CID122413384.
  16. ^Sekanina, Zdenek; Chodas, Paul W. (10 December 2002)."Common Origin of Two Major Sungrazing Comets".The Astrophysical Journal.581(1): 760–769.Bibcode:2002ApJ...581..760S.doi:10.1086/344216.
  17. ^Kimura, H (October 2002). "Dust Grains in the Comae and Tails of Sungrazing Comets: Modeling of Their Mineralogical and Morphological Properties".Icarus.159(2): 529–541.Bibcode:2002Icar..159..529K.doi:10.1006/icar.2002.6940.
  18. ^cometography.com,C/1979 Q1 – SOLWIND 1
  19. ^Sekanina, Zdeněk; Chodas, Paul W. (2007)."Fragmentation Hierarchy of Bright Sungrazing Comets and the Birth and Orbital Evolution of the Kreutz System. II. The Case for Cascading Fragmentation".The Astrophysical Journal.663(1): 657–676.Bibcode:2007ApJ...663..657S.doi:10.1086/517490.hdl:2014/40925.
  20. ^abSekanina, Zdenek; Kracht, Rainer (8 May 2014). "Disintegration of Comet C/2012 S1 (ISON) Shortly Before Perihelion: Evidence From Independent Data Sets".arXiv:1404.5968[astro-ph.EP].
  21. ^"A Unique Hubble View of Comet ISON".Image Gallery.ESA/Hubble.Retrieved15 August2013.
  22. ^Complete list of SOHO comets
  23. ^J. Bortle (2012-09-24)."the orbital elements' distinct and surprising similarity to those of the Great Comet of 1680".comets-ml · Comets Mailing List. Archived fromthe originalon December 9, 2012.Retrieved2012-10-05.
  24. ^Death-defying comet wags its tail during solar embrace

References

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