31 Euphrosyne

31 Euphrosyne
Discovery
Discovered byJ. Ferguson
Discovery dateSeptember 1, 1854
Designations
(31) Euphrosyne
Pronunciation/juːˈfrɒsɪniː/[1]
Named after
Εὐφροσύνη Eyphrosynē
A907 GP; A918 GB
Main belt
AdjectivesEuphrosynean /juːfrɒsɪˈniːən/[2]
Orbital characteristics[3]
Epoch April 27, 2019 (JD 2458600.5)
Aphelion3.8523 AU
(576.296 Gm)
Perihelion2.4585 AU
(367.786 Gm)
3.1554 AU
(472.041 Gm)
Eccentricity0.2209
5.61 yr (2041.585 d)
87.1671°
Inclination26.3033°
31.1186°
61.4704°
Known satellites1
Physical characteristics
Dimensionsc/a = 0.86±0.07[4]
(294±6) × (280±10) × (248±6) km[5]
268±4 km[4]
267.1±2.6 km (IRAS)[3]
268±6 km[5]
Mass(16.5±2.6)×1018 kg[4]
(17±3)×1018 kg[5]
Mean density
1.64±0.27 g/cm3[4]
1.66±0.24 g/cm3[5]
0.230400 d (5.529595 h)[5]
0.05[4]
0.0543[6]
C[3][7]
10.16[8] to 13.61
6.74[3]

31 Euphrosyne is a very young asteroid. It is one of the largest asteroids (approximately tied for 7th place, to within measurement uncertainties). It was discovered by James Ferguson on September 1, 1854, the first asteroid found from North America. It is named after Euphrosyne, one of the Charites in Greek mythology. In 2019 a small companion was discovered. It is the third-roundest known asteroid (after 1 Ceres and 10 Hygiea); this is thought to be due to having re-accreted after being disrupted by a collision, and it is not close to hydrostatic equilibrium.[5]

Observations

Euphrosyne is a fairly dark body near the belt's outer edge. Consequently, it is never visible with binoculars, having a maximum apparent magnitude at the best possible opposition of around +10.2 (as in November 2011), which is fainter than any of the thirty asteroids previously discovered.[9]

Euphrosyne has a high orbital inclination and eccentricity having nodes near perihelion and aphelion, Euphrosyne's perihelion lies at the northernmost point of its orbit. During perihelic oppositions, Euphrosyne is very high in the sky from northern latitudes and invisible from southern countries such as New Zealand and Chile.

Surface

Euphrosyne is a C-type asteroid with a primitive surface possibly covered by thick ejecta blanket from the collision that created its moon and collisional family. There are no deep basins. Any craters larger than 40 km in diameter must have flat floors to not be visible in the VLT images, consistent with an icy C-type composition. The lack of craters could also be due to the young age of the surface.[5]

Mass and density

The discovery of its satellite enabled the first accurate measure of Euphrosyne's mass in 2020, at (1.7±0.3)×1019 kg, and thus a density of 1.7±0.2 g/cm3. The low density suggests that Euphrosyne is half water ice if internal porosity is 20%.[5]

Family

Euphrosyne is the namesake of a complex family of about two thousand asteroids that share similar spectral properties and orbital elements. They are thought to have arisen from a recent collision approximately 280 million years ago.[5] All members have relatively high orbital inclinations.[10] The second largest body in this group, 895 Helio, is most likely an interloper.[11]

Satellite

S/2019 (31) 1
Discovery
Discovery date2019 March 15
Designations
Designation
Euphrosyne I
Orbital characteristics[5]
Epoch EQJ2000
672±12 km
Eccentricity0.043+0.041
−0.014
1.209±0.001 days
Inclination1.4°±0.5°
80.1°±9.3°
135.2°±13.5°
Physical characteristics
4.0±1.0 km

In 2019 a small satellite was discovered, likely resulting from the same collisional event that created the family. Preliminary orbit computations indicated an orbital period of approximately 1.2 days and a semi-major axis of 670 km. VLT images indicate that the moon is 4 km in diameter, assuming it has the same albedo as Euphrosyne.[5]

Asteroid Euphrosyne—time-lapse view by WISE (May 17, 2010)

References

  1. ^ Noah Webster (1884) A Practical Dictionary of the English Language
  2. ^ "Elia", The New-England Magazine, vol. IX, Oct. 1835, p. 236
  3. ^ a b c d "JPL Small-Body Database Browser: 31 Euphrosyne" (2018-06-15 last obs). Retrieved 28 April 2019.
  4. ^ a b c d e P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
  5. ^ a b c d e f g h i j k Yang, B.; et al. (September 2020), "Binary asteroid (31) Euphrosyne: ice-rich and nearly spherical", Astronomy & Astrophysics, 641: 9, arXiv:2007.08059, Bibcode:2020A&A...641A..80Y, doi:10.1051/0004-6361/202038372, A80
  6. ^ "Albedo table". Archived from the original on 22 July 2012. Retrieved 27 December 2006.
  7. ^ "Astrometric and Geodetic Properties of Earth and the Solar System" (PDF). Archived from the original (PDF) on 7 July 2009. Retrieved 6 August 2007.
  8. ^ "Bright Minor Planets 2000". Minor Planet Center. Retrieved 23 May 2008.[permanent dead link‍]
  9. ^ "Brightest asteroids". Archived from the original on 7 February 2012. Retrieved 6 August 2007.
  10. ^ Novaković, Bojan; et al. (November 2011), "Families among high-inclination asteroids", Icarus, 216 (1): 69–81, arXiv:1108.3740, Bibcode:2011Icar..216...69N, doi:10.1016/j.icarus.2011.08.016.
  11. ^ Yang, B.; et al. (November 2020), "Physical and dynamical characterization of the Euphrosyne asteroid family", Astronomy & Astrophysics, 643: 9, arXiv:2009.04489, Bibcode:2020A&A...643A..38Y, doi:10.1051/0004-6361/202038567, A38