Comet Arend–Roland

C/1956 R1 (Arend–Roland)

Discovery
Discovered by:	Sylvain Arend, Georges Roland
Discovery date:	1956
Alternate designations:	1957 III, 1956h, C/1956 R1
Orbital characteristics A
Epoch:	2435920.5 (March 23, 1957)
Aphelion distance:	N/A
Perihelion distance:	0.31604 AU
Semi-major axis:	45,000 AU
Eccentricity:	1.00024[1] 1.000199 (epoch 1977+)[2]
Orbital period:	N/A
Inclination:	119.94°
Last perihelion:	April 8, 1957
Next perihelion:	ejection

Comet Arend–Roland was discovered on November 8, 1956, by Belgian astronomers Sylvain Arend and Georges Roland on photographic plates. As the eighth comet found in 1956, it was named Arend–Roland 1956h after its discoverers. Because it was the third comet to pass through perihelion during 1957, it was then renamed 1957 III.^[3] Finally, it received the standard IAU designation C/1956 R1 (Arend–Roland), with the 'C/' indicating it was a non-periodic comet and the R1 showing it was the first comet reported as discovered in the half-month designated by R. The last is equivalent to the period September 1–15.^[4]

Observations

In November 1956, a double astrograph at the Uccle Observatory in Brussels was being used for routine investigation of minor planets. On November 8, 1956, the Belgian astronomers Sylvain Arend and Georges Roland discovered a comet on their photographic plates. At that time the comet was at visual magnitude 10, with a strong central condensation and a short tail. The early discovery of this comet allowed observing programs and equipment to be prepared well in advance.^[5]

The orbital elements for this comet were computed by Michael P. Candy, who predicted perihelion passage on April 8, 1957. As the comet was already well developed, he predicted that the object would present a prominent display during the month of April in the northern hemisphere. In early December the comet was 2.5 AU from the Sun and 1.7 AU from the Earth. It was in the constellation Pisces until February, when it reached magnitude 7.5–8.^[5]

During the April perihelion passage, the tail of the comet reached a length of 15° of arc. The appearance of the tail varied, with streamers on April 16 and May 5, and the tail splitting into three beams on the 29th. By April 22 the comet also displayed a prominent anomalous tail (or antitail) spanning 5°. This antitail stretched out to span 12° on April 25,^[6] reaching its maximum extent. The antitail had disappeared by April 29.^[7]

Following perihelion, the comet began to fade rapidly. At the start of May it was measured at visual magnitude 5.46. By the eighth it had decreased to magnitude 7, well below the sensitivity limit of the unaided human eye. On May 29 it had dropped to magnitude 8.55.^[8]

This was the first comet that attempts were made to detect it at various radio frequencies. However, these efforts were unsuccessful. A comet would not be successfully detected in the radio band until the 1973 passage of comet Kohoutek.^[9]

Comet Arend–Roland was the subject of the very first edition of the BBC's long running astronomy program The Sky at Night on April 24, 1957.^[10]

Astronomer Carl Sagan relates an anecdote on page 80 of his book Cosmos about being on duty in an observatory near Chicago in 1957 when a late night phone call from an inebriated man asked what was the "fuzzy thing" they were seeing in the sky. Sagan told the man it was a comet (Arend–Roland). The man asked what a comet was, and Sagan answered that it was "a snowball, one mile wide". After a long pause, the man said, quoting Sagan: "Lemme talk to a real 'shtronomer!".

Properties

It was traveling on a hyperbolic orbit, meaning it is traveling fast enough to escape from the solar system entirely, hence implying it will never be seen again by earthbound observers. Observations of the comet over a period of 520 days allowed precise orbital elements to be computed. However, the distribution of the orbital elements showed a wavy pattern that suggested a non-gravitational influence. Alternatively, the comet may have originated from interstellar space rather than from the Oort cloud.^[11] When an orbital solution is computed that includes non-gravitational forces that vary as the inverse square of the heliocentric distance, somewhat different values are derived. (See the Marsden (1970) column in the table below.)^[12]

Orbital Element	Sekanina (1968)[11]	Marsden (1970)[12]
Epoch of periastron (T)	1957 April 8.03232 ET	1957 April 8.03201 ET
Perihelion distance (q)	0.3160540 ± 0.0000008 AU	0.3160361 ± 0.0000024 AU
Inverse semi-major axis (1/a)	–0.0007886 ± 0.0000045 AU−1	–0.0006377 ± 0.0000213 AU−1
Eccentricity (e)	1.0002492 ± 0.0000014	1.0002015 ± 0.0000067
Inclination (i)	119.94936° ± 0.00005°	119.94930° ± 0.00006°
Longitude of periastron (ω)	307.78084° ± 0.00004°	308.77725° ± 0.00048°
Position angle of the ascending node (Ω)	215.15900° ± 0.00006°	215.15968° ± 0.00008°

At perihelion, the comet was emitting an estimated 7.5 × 10⁴ kg/s of dust and was releasing roughly 1.5 × 10³⁰ molecules/sec gas molecules. It is believed that an outburst of dust occurred on April 2, six days before perihelion. The antitail was formed from particles released between February 6 and March 1, 1957.^[13] Estimates of the total amount of dust released into the zodiacal cloud range from 3 × 10⁸ to 5 × 10¹⁰ kg.^[14]

References

1. ^ "JPL Small-Body Database Browser: C/1956 R1 (Arend–Roland)". Jet Propulsion Laboratory. 1958-04-11 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=C/1956+R1. Retrieved 2011-03-13. 
2. ^ Horizons output. "Barycentric Osculating Orbital Elements for Comet C/1956 R1 (Arend–Roland)". http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=C/1956+R1. Retrieved 2011-03-12.  (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
3. ^ Kaler, James B. (2002). The ever-changing sky: a guide to the celestial sphere. Cambridge University Press. p. 358. ISBN 0521499186. 
4. ^ "Cometary Designation System". IAU Minor Planet Center (Center for Astrophysics, Harvard University). http://www.minorplanetcenter.org/iau/lists/CometResolution.html. Retrieved 2009-09-15. 
5. ^ ^{a b} Hendrie, M. J. (December 1996). "The two bright comets of 1957". Journal of the British Astronomical Association 106 (6): 315–330. Bibcode 1996JBAA..106..315H. 
6. ^ Larsson-Leander, G. (1959). "Physical observations of Comet Arend–Roland (1956 h)". Arkiv för Astronomii 2: 259–271. Bibcode 1959ArA.....2..259L. 
7. ^ Whipple, Fred L. (1957-06-15). "The Sunward Tail of Comet Arend–Roland". Nature 179 (1240): 1240. Bibcode 1957Natur.179.1240W. doi:10.1038/1791240a0. 
8. ^ Wehlau, Amelia; Wehlau, William (1959). "Photoelectric photometry of Comet Arend–Roland (1956h)". Astronomical Journal 64: 463–467. Bibcode 1959AJ.....64..463W. doi:10.1086/107974. 
9. ^ Altenhoff, W. J.; et al. (2002). "Radio continuum observations of Comet C/1999 S4 (LINEAR) before, during, and after break-up of its nucleus". Astronomy & Astrophysics 391 (1): 353–360. Bibcode 2002A&A...391..353A. doi:10.1051/0004-6361:20020783. 
10. ^ Moore, Patrick. "A History of The Sky at Night". BBC. http://www.bbc.co.uk/science/space/skyatnight/patrickmoore_article2.shtml. Retrieved 2009-09-15. 
11. ^ ^{a b} Sekanina, Z. (1968). "A dynamic investigation of Comet Arend–Roland 1957 III". Bulletin of the Astronomical Institute of Czechoslovakia 19: 343–350. Bibcode 1968BAICz..19..343S. 
12. ^ ^{a b} Marsden, B. G. (February 1970). "Comets and Nongravitational Forces. III". Astronomical Journal 75: 75–84. Bibcode 1970AJ.....75...75M. doi:10.1086/110945. 
13. ^ Finson, M.; Probstein, R. (1968). "A Theory of Dust Comets. II. Results for Comet Arend–Roland". Astrophysical Journal 154: 353–380. Bibcode 1968ApJ...154..327F. doi:10.1086/149761. 
14. ^ Fulle, M. (January 1988). "Meteoroids from comets Arend–Roland 1957III and Seki-Lines 1962III". Astronomy and Astrophysics 189 (1–2): 281–291. Bibcode 1988A&A...189..281F. 

External links

• Orbital simulation from JPL (Java) / Ephemeris
• C/1956 R1 (Arend–Roland)
• Picture of Antitail