Astronomy:163 Erigone

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Short description: Main-belt asteroid
163 Erigone
000163-asteroid shape model (163) Erigone.png
3D convex shape model of 163 Erigone
Discovery
Discovered byJ. Perrotin
Discovery siteToulouse
Discovery date26 April 1876
Designations
(163) Erigone
Pronunciation/ɪˈrɪɡəniː/[1]
Named afterErigone
A876 HC; 1892 RA;
1957 OT; 2017 YH23
Minor planet categoryMain belt (Erigone)
AdjectivesErigonian /ɛrɪˈɡoʊniən/[2] Erigonean /ɛrɪɡəˈniːən/
Orbital characteristics[3]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc123.56 yr (45131 d)
|{{{apsis}}}|helion}}2.8188 astronomical unit|AU (421.69 Gm)
|{{{apsis}}}|helion}}1.9161 AU (286.64 Gm)
2.3675 AU (354.17 Gm)
Eccentricity0.19064
Orbital period3.64 yr (1330.5 d)
Mean anomaly280.031°
Mean motion0° 16m 14.052s / day
Inclination4.8148°
Longitude of ascending node160.166°
298.260°
Earth MOID0.93686 AU (140.152 Gm)
Jupiter MOID2.3628 AU (353.47 Gm)
TJupiter3.518
Physical characteristics
Dimensions72.63±5.7 km[3]
72.70 ± 1.95 km[4]
Mass(2.01 ± 0.68) × 1018 kg[4]
Mean density9.99 ± 3.45 g/cm3[4]
Rotation period16.136 h (0.6723 d)[5]
Geometric albedo0.0546±0.010[3]
0.0428 ± 0.0092 [6]
C[6] (Tholen)
Absolute magnitude (H)9.47,[3] 9.48[6]


163 Erigone is an asteroid from the asteroid belt and the namesake of the Erigone family of asteroids that share similar orbital elements and properties. It was discovered by French astronomer Henri Joseph Perrotin on April 26, 1876, and named after one of the two Erigones in Greek mythology. This asteroid is orbiting the Sun at a distance of 2.37 astronomical unit|AU with a period of 3.643 years and an eccentricity (ovalness) of 0.19. The orbital plane is inclined at an angle of 4.8° to the plane of the ecliptic.[3]

Photometric measurements taken in 2014 were used to construct a lightcurve that demonstrated a rotation period of 16.136±0.001 h with an amplitude of 0.32±0.02 in magnitude.[5] Erigone is a relatively large and dark asteroid with an estimated size of 73 km.[4] Based upon its spectrum, it is classified as a C-type asteroid,[6] which indicates that it probably has a carbonaceous composition. It is the largest member of the eponymously named Erigone collisional family.[7]

2014 occultation of Regulus

Path of occultation from New York to Ontario

In the early morning hours of March 20, 2014, Erigone occulted the first-magnitude star Regulus,[8] as first predicted by Aldo Vitagliano in 2004 using the SOLEX software.[9] This would have been a rare case of an occultation of a very bright star visible from a highly populated area, since the shadow path moved across New York state and Ontario, including all five boroughs of New York City .[9] Observers in the shadow path would have seen the star wink out for as long as 14 seconds.[8][10]

However, thick clouds and rain blocked the view for most if not all people on the shadow path.[11] The website of the International Occultation Timing Association does not list any successful observations at all.[12]

Two single chord Asteroid Occultation events have been observed, in 2013 and 2015.[13]

References

  1. ↑ Noah Webster (1884) A Practical Dictionary of the English Language
  2. ↑ Publius Ovidius Naso, John Gower (1640) Ovids Festivalls
  3. ↑ 3.0 3.1 3.2 3.3 3.4 "163 Erigone". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=163;cad=1. 
  4. ↑ 4.0 4.1 4.2 4.3 Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science 73 (1): 98–118, doi:10.1016/j.pss.2012.03.009, Bibcode: 2012P&SS...73...98C.  See Table 1.
  5. ↑ 5.0 5.1 Pilcher, Frederick et al. (July 2014). "Rotation Period Determination for 163 Erigone". Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers 41 (3): 187. Bibcode: 2014MPBu...41..187P. 
  6. ↑ 6.0 6.1 6.2 6.3 Pravec, P. et al. (May 2012), "Absolute Magnitudes of Asteroids and a Revision of Asteroid Albedo Estimates from WISE Thermal Observations", Asteroids, Comets, Meteors 2012, Proceedings of the conference held May 16–20, 2012 in Niigata, Japan 1667 (1667): pp. 6089, Bibcode: 2012LPICo1667.6089P.  See Table 4.
  7. ↑ Morate, David et al. (February 2016), "Compositional study of asteroids in the Erigone collisional family using visible spectroscopy at the 10.4 m GTC", Astronomy and Astrophysics 586: 18, doi:10.1051/0004-6361/201527453, A129, Bibcode: 2016A&A...586A.129M. 
  8. ↑ 8.0 8.1 Dunham, David (2006). "The International Occultation Timing Association 24th Annual Meeting at Mt. Cuba Observatory, Greenville, Delaware". International Occultation Timing Association. Archived from the original on 2011-07-18. https://web.archive.org/web/20110718013258/http://www.weblore.com/richard/IOTAMeeting2006.htm. Retrieved 2011-02-13. 
  9. ↑ 9.0 9.1 Vitagliano, Aldo (2010). "The Solex Page". Università degli Studi di Napoli Federico II. Archived from the original on 2008-12-20. https://web.archive.org/web/20081220235836/http://chemistry.unina.it/~alvitagl/solex/. Retrieved 2011-02-13. 
  10. ↑ Preston, Steve (2014-03-14). "(163) Erigone / HIP 49669". Asteroid Occultation. Archived from the original on 2013-12-24. https://web.archive.org/web/20131224171236/http://www.asteroidoccultation.com/2014_03/0320_163_32317_Summary.txt. Retrieved 2014-03-14. 
  11. ↑ Asteroid eclipse rained out Space.com 2014 March 20
  12. ↑ Regulus 2014 International Occultation Timing Association
  13. ↑ "PDS Asteroid/Dust Subnode" (in en). https://sbn.psi.edu/pds-staging/resource/occ.html. 

External links

vec:Lista de asteroidi#163 Erigona



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