(386723) 2009 YE7
|Discovered by||David Rabinowitz|
|Discovery date||17 December 2009|
|MPC designation||2009 YE7|
|Epoch 13 January 2016 (JD 2457400.5)|
|Uncertainty parameter 4|
|Observation arc||2273 days (6.22 yr)|
|Aphelion||50.694 AU (7.5837 Tm) (Q)|
|Perihelion||37.893 AU (5.6687 Tm) (q)|
|44.293 AU (6.6261 Tm) (a)|
|294.79 yr (107672 d)|
Average orbital speed
|0° 0m 12.037s / day (n)|
|Earth MOID||37.0065 AU (5.53609 Tm)|
|Jupiter MOID||33.2361 AU (4.97205 Tm)|
|Jupiter Tisserand parameter||5.164|
|assume 0.7 to 0.09|
|Temperature||< 44 K|
(386723) 2009 YE7 is a classical Kuiper belt object: Its orbit is not controlled by an orbital resonance with Neptune, similar to (15760) 1992 QB1, but with a much greater orbital eccentricity and inclination. It completes one orbit around the Sun in just over 247 Earth years, at an average distance of about 44 AU. It came to perihelion around 1868, and to aphelion in 2015. It is currently about 50.7 AU from the Sun, and will again return to perihelion around 2163.
(386723) 2009 YE7 has been observed 70 times, with precovery images dating back to 2006, and has an orbital quality code of 4.
The size of an object can be ascertained once its absolute magnitude (H) and its albedo (the proportion of light it reflects) are known. When (386723) 2009 YE7 was first discovered, it was believed to have an absolute magnitude (H) of 2.8, which would have made it the first bright KBO found from the southern hemisphere.(386723) 2009 YE7 has an absolute magnitude (H) of 4.25. Since (386723) 2009 YE7 has an absolute magnitude dimmer than (H=1), it will not be overseen by two naming committees and will not automatically be listed as a dwarf planet by the International Astronomical Union (IAU). This value would've made it the eighth-intrinsically-brightest known trans-Neptunian object, but it was later found to be much dimmer. It has an absolute magnitude (H) of 4.25., which would make it a good dwarf-planet candidate when using an albedo of 0.09. However, it is probably much smaller than previously thought, since it is also suspected of being a highly reflective icy member of the Haumea family.
(386723) 2009 YE7 has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detection of water ice on its surface. This means (386723) 2009 YE7 could have an albedo of up to 0.7, resulting in a small size close to 200 kilometres (120 mi). However, its actual albedo is unknown; if its albedo turns out to be lower, it would result in a larger size estimate.
- (55636) 2002 TX300, known Haumea-family member
- Spitzer dwarf-planet candidates with estimated diameter > 600 kilometres (370 mi)
- List of Solar System objects most distant from the Sun in 2015
- "List of Transneptunian Objects". IAU Minor Planet Center. 2009-12-28. Retrieved 2009-12-28.
- "2009 YE7 Orbit". IAU Minor Planet Center. Retrieved 2014-04-02.
- Trujillo; Sheppard & Schaller (14 February 2011). "A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects". The Astrophysical Journal. arXiv:1102.1971. Bibcode:2011ApJ...730..105T. doi:10.1088/0004-637X/730/2/105.
- Mike Brown (2009-12-29). "A ghost of Christmas past". Mike Brown's Planets (blog). Archived from the original on 2 January 2010. Retrieved 2009-12-29.
- "JPL Small-Body Database Browser: 386723 (2009 YE7)" (last observation: 2010-09-12). Retrieved 12 April 2016.
- Assuming a Haumea-like albedo of 0.7
- Assuming an unlikely albedo of 0.09
- Dan Bruton. "Conversion of Absolute Magnitude to Diameter for Minor Planets". Department of Physics & Astronomy (Stephen F. Austin State University). Archived from the original on 18 December 2008. Retrieved 2009-01-07.
- "JPL Small-Body Database Search Engine (H<=4)". 2009-12-27. Retrieved 2009-12-27.
- "Plutoid chosen as name for Solar System objects like Pluto" (Press release). Retrieved 28 December 2009.
- Mike Brown. "The Dwarf Planets". Archived from the original on 9 January 2010. Retrieved 2009-12-28.
- Orbital simulation from JPL (Java) / Horizons Ephemeris
- (386723) 2009 YE7 at the JPL Small-Body Database