C/1979 Y1 (Bradfield)

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C/1979 Y1 (Bradfield)
Comet Brandfield 6-2-1980 3 00 (UT) by JOCR.jpg
Negative image of the comet on 6 February 1980
Discovery [1]
Discovered by William A. Bradfield
Discovery site Dernancourt, South Australia
Discovery date24 December 1979
Designations
1979l [2]
1979 X
Orbital characteristics [3] [4]
Epoch 25 January 1980 (JD 2444263.5)
Observation arc 75 days
Number of
observations		127
Aphelion 91 ± 1 AU
Perihelion 0.5453 AU
Semi-major axis 46 AU
Eccentricity 0.988
Orbital period 308 ± 6 years
Avg. orbital speed 67.98 km/s
Inclination 148.602°
103.216°
Argument of
periapsis 		257.609°
Last perihelion21 December 1979
Next perihelion≈2287?
TJupiter –0.665
Earth MOID 0.0671 AU
Jupiter MOID 1.6930 AU
Physical characteristics
Comet total
magnitude (M1)		8.5
5.0
(1980 apparition)

C/1979 Y1 (Bradfield), also known as Comet 1979X and 1979l, is a long period comet discovered by William A. Bradfield on 24 December 1979. The comet has an orbital period of 308 ± 6 years and last passed perihelion on 21 December 1979. It is considered to be the parent body of the July Pegasids meteor shower. It is expected to next come to perihelion around 2287. [4]

Contents

Observational history

The comet was discovered by amateur astronomer William A. Bradfield on 24 December 1979, using a 150mm f5.5 refractor at Dernancourt, South Australia. It was the 10th comet discovered by Bradfield, who had been searching for 67 hours following the discovery of his previous comet. [5] The comet was discovered three days after perihelion and was estimated to have an apparent magnitude of 5. Bradfield also reported it had a tail over a degree long. [1] The comet was then located in the constellation of Scorpius and moving southwards. [6]

In January the comet remained around magnitude 5, as it was approaching Earth. On 8 January its tail was reported to be three degrees long as seen by 15×80 binoculars, while by 17 January it was reported to be two degrees long. The comet was moving southwards until 23 January, when it reached a declination of -80°, and consequently moved rapidly northwards, becoming visible from the northern hemisphere on 26 January, when the comet was 0.2 AU from Earth. [7] On 6 February the ion tail of the comet appeared to undulate, shifting its axis by about 10 degrees in 27 minutes, due to a solar wind disturbance. [8] [9] In February the comet faded as it moved away from Earth and its tail became shorter, being 5 arcminutes long on 18 February. The comet was last detected on 17 March 1980, when it had an apparent magnitude of 11.7. [7]

Scientific results

Ultraviolet observations

The comet was favorably located in the sky to be observed by the International Ultraviolet Explorer. Comet Bradfield was the third comet whose ultraviolet spectrum was obtained from space after comets C/1975 V1 (West) and C/1978 T1 (Seargent). The observations started on 10 January 1980, when the comet was at an heliocentric distance of 0.71 AU and ended on 3 March 1980, when the comet was at a distance of 1.55 AU. [10] [11]

The most prominent feature was the Lyman-alpha line of the hydrogen, which appeared overexposed. Other lines observed were the OI λ1302, CI λλ1561, 1637 and 1931, and SI λ1813, while just over the noise level are the CII complex and CO. The ultraviolet spectrum was very similar to comet West, despite the difference in gas to dust ratio. In longer wavelengths were observed CO+, CO+2, CS and OH bands, however the CO+ (0,0) and (1,0) lines were very weak or absent. [10] The CS and SI lines appear concentrated near the nucleus of the comet. [12]

The OH and hydrogen lines are the result of the photodissociation of water due to the solar radiation. It is possible that in the hydrogen component contribute and other molecules, but not as much. OH is further dissociated to hydrogen and oxygen. The water production at 0.71 AU was estimated to be 1–2.4 × 1029 mol/s. The vaporisation of water was decreasing at a rate of r−3.7. [11] The absence of some of the CO+ lines was considered surprising, while it was the first time CII Mulliken bands were unambiguously present in a comet. [13] The presence of CS and sulfur is attributed to the photodissociation of carbon disulfide. [12]

Other wavelengths

The spectrum of the comet in the visible light was obtained between 4–12 February 1980 by the Asiago Astrophysical Observatory. It revealed the presence of CN, C2, C3, NH2 and CH bands, while in the near infrared were observed the (3-0) Philipps band system of C2 and the (8-0), (7-0), (6-0) bands of H2O(+). [14] The comet was also observed in near infrared on 29 January by the ESO with a spectrograph attached to 3.6 m telescope in spectral region between λ6600 and λ 11000. The spectrum revealed the presence of CN 2–0, 3–1, and 1-0 bands in the nucleus and CN 1-0 and 2-0 bands in the coma. Other lines present in the spectrum were the OI λ6300 and 6364 lines, and the NH2 sequence. The spectrum was similar to that of comet C/1969 T1 (Tago–Sato–Kosaka), although the NH2 line was relatively weaker. [15]

It was attempted to observe the emission of HCN, CS, and CH3OH in millimeter wavelengths, but was unsuccessful. [16] In radiowaves there was conducted an unsuccessful search for hydroxyl radical, formaldehyde (H2CO), methyl formate (HCOOCH3), water, ammonia and a hydrogen recombination line, indicating a water production rate below ~7.4×1030 molecules/s. [17]

There was also an attempt to image the comet in soft X-rays using the Einstein Observatory on 5 February 1980, but no X-ray emission was detected. [18]

Meteor showers

The comet is considered to be the parent body of the July Pegasids meteor shower, a weak meteor shower. Comet C/1771 A1 has also being suggested to be the parent body of that shower and it could be possible that both C/1979 Y1 and C/1771 A1 were created by a single progenitor comet, which also created the Pegasids shower. [19] Modeling of the meteor streams of the comet also suggests they create a daylight meteor shower too, with the radiant point in the constellation of Microscopium, near alpha Microscopii. It could also be the parent body of γ-Bootids, a meteor shower whose existence, however, is questionable, as it was identified by only two meteors. The streams that cause the Pegasids and daylight showers are dragged away from Earth's orbit due to the Poynting–Robertson effect, while the γ-Bootids are dragged into it. [20]

Comet Bradfield could also produce a meteor shower on Mars, visible in the morning in the south hemisphere. The comet has a lower minimum orbit intersection distance with Mars than Earth, at 0.0497 AU (7.44 million km; 4.62 million mi). [21]

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References

  1. 1 2 D. W. Green (26 December 1979). "Comet Bradfield (1979l)". Central Bureau for Astronomical Telegrams. 3437.
  2. ↑ "Comet Names and Designations". International Comet Quarterly. Retrieved 1 December 2024.
  3. ↑ "C/1979 Y1 (Bradfield) – JPL Small-Body Database Lookup". ssd.jpl.nasa.gov. Jet Propulsion Laboratory . Retrieved 1 December 2024.
  4. 1 2 "Horizons Batch for Bradfield (C/1979 Y1) (90002034) in 2287" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons . Retrieved 26 August 2023. (JPL#9 / Soln.date: 2021-Apr-15)
  5. ↑ K. Thalassoudis. "Comets Discovered from South Australia". www.assa.org.au. Astronomical Society of South Australia. Retrieved 10 March 2023.
  6. ↑ B. G. Marsden (March 1985). "Comets in 1979". Quarterly Journal of the Royal Astronomical Society. 26: 106–114. Bibcode:1985QJRAS..26..106M. ISSN   0035-8738.
  7. 1 2 B. G. Marsden (June 1985). "Comets in 1980". Quarterly Journal of the Royal Astronomical Society. 26: 156–167. Bibcode:1985QJRAS..26..156M. ISSN   0035-8738.
  8. ↑ J. C. Brandt; J. D. Hawley; M. B. Niedner (October 1980). "A very rapid turning of the plasma-tail axis of comet Bradfield 19791 on 1980 February 6". The Astrophysical Journal. 241: L51. Bibcode:1980ApJ...241L..51B.
  9. ↑ J. F. Le Borgne (June 1983). "Interpretation of the event in the plasma tail of comet Bradfield 1979 X on 1980 February 6". Astronomy and Astrophysics. 123 (1): 25–28. Bibcode:1983A&A...123...25L. ISSN   0004-6361.
  10. 1 2 P. D. Feldman; H. A. Weaver; M. C. Festou; M. F. A'Hearn; W. M. Jackson; et al. (July 1980). "IUE observations of the UV spectrum of comet Bradfield". Nature . 286 (5769): 132–135. Bibcode:1980Natur.286..132F. doi:10.1038/286132a0. hdl: 2027.42/62727 . S2CID   4334030.
  11. 1 2 H. A. Weaver; P. D. Feldman; M. C. Festou; M. F. A'Hearn (December 1981). "Water production models for comet Bradfield /1979 X/". The Astrophysical Journal . 251: 809. Bibcode:1981ApJ...251..809W. doi:10.1086/159525.
  12. 1 2 W. M. Jackson; J. B. Halpern; P. D. Feldman; J. Rahe (March 1982). "Production of CS and S in Comet Bradfield /1979 X/". Astronomy and Astrophysics. 107 (2): 385–389. Bibcode:1982A&A...107..385J. ISSN   0004-6361.
  13. ↑ M. F. Ahearn; P. D. Feldman (December 1980). "Carbon in Comet Bradfield 1979l". The Astrophysical Journal . 242: L187. Bibcode:1980ApJ...242L.187A. doi: 10.1086/183429 .
  14. ↑ C. B. Cosmovici; S. Ortolani (August 1980). "Spectroscopic and photographic observations of Comet Bradfield /1979-l/". Astronomy and Astrophysics. 88 (3): L16 –L20. Bibcode:1980A&A....88L..16C. ISSN   0004-6361.
  15. ↑ A. C. Danks; M. Dennefeld (February 1981). "Near-infrared spectroscopy of comet Bradfield 1979l". The Astronomical Journal. 86: 314. Bibcode:1981AJ.....86..314D. doi: 10.1086/112890 .
  16. ↑ L. Ekelund; W. M. Irvine; C. Andersson; F. P. Schloerb; S. E. Robinson (September 1981). "A search for millimeter-wave emission from HCN and other molecules in Comet Bradfield (1979l)". Icarus . 47 (3): 431–433. Bibcode:1981Icar...47..431E. doi:10.1016/0019-1035(81)90190-1.
  17. ↑ J. M. Hollis; J. C. Brandt; R. W. Hobbs; S. P. Maran; P. D. Feldman (February 1981). "Radio observations of Comet Bradfield /1979l/". The Astrophysical Journal. 244: 355. Bibcode:1981ApJ...244..355H. doi: 10.1086/158713 .
  18. ↑ H. S. Hudson; W. H. Ip; D. A. Mendis (December 1981). "A Search for X-ray emission from comet Bradfield (1979l)". Planetary and Space Science. 29 (12): 1373–1376. doi:10.1016/0032-0633(81)90104-5.
  19. ↑ D. Holman; P. Jenniskens (April 2013). "Discovery of the Upsilon Andromedids (UAN, IAU #507)". WGN, Journal of the International Meteor Organization. 41 (2): 43–47. Bibcode:2013JIMO...41...43H. ISSN   1016-3115.
  20. ↑ M. Hajduková; L. Neslušan (September 2017). "Regular and transitory showers of comet C/1979 Y1 (Bradfield)". Astronomy & Astrophysics. 605: A36. Bibcode:2017A&A...605A..36H. doi: 10.1051/0004-6361/201730646 .
  21. ↑ A. A. Christou (March 2010). "Annual meteor showers at Venus and Mars: Lessons from the Earth". Monthly Notices of the Royal Astronomical Society. 402 (4): 2759–2770. Bibcode:2010MNRAS.402.2759C. doi: 10.1111/j.1365-2966.2009.16097.x .
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