341520 Mors–Somnus
| Discovery | |
|---|---|
| Discovered by | Scott S. Sheppard and C. Trujillo |
| Discovery date | October 14, 2007 |
| Designations | |
| MPC designation | 341520 Mors–Somnus |
| Plutino[1] | |
| Orbital characteristics[2] | |
| Epoch 2016-Jan-13.0 (JD 2457400.5) | |
| Aphelion | 49.400 AU |
| Perihelion | 28.840 AU |
| 39.120 AU | |
| Eccentricity | 0.263 |
| 244.68 a (89370.137 d) | |
| 357.860° | |
| Inclination | 11.300 ° |
| 196.743° | |
| 205.665° | |
| Physical characteristics | |
| Dimensions | <60 km (each component)[1] |
| Mass | 7.90 ± 0.21×1017 kg |
Mean density | >0.5 g/cm3[1] |
Sidereal rotation period | 9.28 h[3] |
| Albedo | >0.17[1] |
Spectral type |
V−R=0.74 ± 0.01, B−R=2.03 ± 0.01[1] |
| 6.94 ± 0.02[1] | |
|
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' 341520 Mors–Somnus also known as 2007 TY430 is a trans-Neptunian object (TNO) that resides in the Kuiper belt and was discovered on October 14, 2007 by Scott S. Sheppard and C. Trujillo with Subaru telescope at Mauna Kea.[2] It is classified as a plutino, which means that it is in the 3:2 mean motion resonance with Neptune.[1]
Naming
341520 Mors–Somnus was named on June 2, 2015 after the mythological Roman god of the underworld and death.[4]
Orbit and binarity
341520 Mors–Somnus is a small double plutino occupying the 3:2 mean motion resonance with Neptune. The object is a wide optically resolved binary with the following orbital parameters
| Semi-major axis, km | Eccentricity | Period, d | Inclination, degree |
| 21000 ± 160 | 0.1529 ± 0.0028 | 961.2 ± 4.6 | 15.68 ± 0.22 |
The components has almost equal size. The total mass of the system is 7.90 ± 0.21×1017 kg. For a realistic minimal density of 0.5 g/cm3 the albedo is >0.17 and the size of the components is <60 km.[1]
Physical properties
341520 Mors–Somnus has an ultra-red spectrum in the visible and near-infrared parts of the spectrum. The colors of two components are indistinguishable from each other.[1]
341520 Mors–Somnus demonstrates a double-peaked light curve with the period of about 9.28 hours and amplitude of 0.24. This indicates that either primary of secondary has an elongated shape and rotates non-synchronosly.[3]
Evolution
341520 Mors–Somnus system is likely to be an escaped cold classical Kuiper Belt object.[1]
References
- 1 2 3 4 5 6 7 8 9 10 11 Scott S. Sheppard; Darin Ragozzine; Chadwick Trujillo (2012). "2007 TY430: A Cold Classical Kuiper Belt Type Binary in the Plutino Population". The Astronomical Journal 143: 58. Bibcode:2012AJ....143...58S. doi:10.1088/0004-6256/143/3/58.
- 1 2 "JPL Small-Body Database Browser: 2007_TY430" (2010-10-04 last obs.). Retrieved 2016-02-27.
- 1 2 A. Thirouin; K. S. Noll; J. L. Ortiz; N. Morales (2014). "Rotational properties of the binary and non-binary populations in the trans-Neptunian belt". Astronomy & Astrophysics 569: A3. Bibcode:2014DPS....4642109T. doi:10.1051/0004-6361/201423567.
- ↑ Wm. Robert Johnston. "(341520) Mors–Somnus". Asteroids with Satellites Database—Johnston's Archive. Retrieved 2016-02-27.
External links
- Orbital simulation from JPL (Java) / Horizons Ephemeris
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