(145480) 2005 TB190

Last updated
(145480) 2005 TB190
145480-2005tb190 hst.jpg
Hubble Space Telescope image of 2005 TB190 taken in 2011
Discovery [1]
Discovered by Becker, A. C., Puckett, A. W., Kubica, J at Apache Point (705)
Discovery date11 October 2005
Designations
(145480) 2005 TB190
Ext-SDO (DES) [2]
Orbital characteristics [1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 3
Observation arc 5041 days (13.80 yr)
Aphelion 104.14  AU (15.579  Tm) (Q)
Perihelion 46.197 AU (6.9110 Tm) (q)
75.166 AU (11.2447 Tm) (a)
Eccentricity 0.38540 (e)
651.69 yr (238031 d)
359.520° (M)
0° 0m 5.445s / day (n)
Inclination 26.5376° (i)
180.4280° (Ω)
171.47° (ω)
Earth  MOID 45.1927 AU (6.76073 Tm)
Jupiter  MOID 41.2446 AU (6.17010 Tm)
Physical characteristics
Dimensions464±62 km [3]
372.5±37.5 km [4]
12.68  h (0.528  d)
12.68 hours
0.148+0.051
−0.036  [3]
0.12–0.20  [4]
B−V=0.98
V−R=0.56 [5]
4.40±0.11 , [3] 4.6 [1]

    (145480) 2005 TB190 (provisional designation 2005 TB190) is a trans-Neptunian object (TNO) with an absolute magnitude of 4.4. [1]

    Contents

    Orbit

    (145480) 2005 TB190 is located near the "gap", a poorly understood region. Extreme transneptunian object eccentricity vs perihelion.png
    (145480) 2005 TB190 is located near the "gap", a poorly understood region.

    (145480) 2005 TB190 is classified as scattered-extended by the Deep Ecliptic Survey (DES), because its orbit appears to be beyond significant gravitational interactions with Neptune's current orbit. [2] However, if Neptune migrated outward, there would have been a period when Neptune had a higher eccentricity. The aphelion of (145480) 2005 TB190 lies at 104 AU. [4]

    Simulations by Emel’yanenko and Kiseleva in 2007 showed that (145480) 2005 TB190 appears to have less than a 1% chance of being in a 4:1 resonance with Neptune. [6]

    It has been observed 202 times over seven oppositions. [1] It will come to perihelion in January 2017. [1] There are precovery observations dating back to November 2001.

    Physical properties

    In 2010, thermal flux from (145480) 2005 TB190 in the far-infrared was measured by the Herschel Space Telescope. As a result, its size was estimated to lie within a range from 335 to 410 km. [4]

    In the visible light, (145480) 2005 TB190 has a moderately red spectral slope. [5]

    The TNO was found in 2009 to have a rotation period of 12.68 ±3 hours, a common value for trans-Neptunian objects of its size. Similarly-sized (120348) 2004 TY364 has a rotation period of 11.7 ± 3 hours.

    Related Research Articles

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    References

    1. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 145480 (2005 TB190)" (2008-08-29 last observation used). Retrieved 7 April 2016.
    2. 1 2 Marc W. Buie (2008-08-29). "Orbit Fit and Astrometric record for 145480". SwRI (Space Science Department). Retrieved 2009-01-24.
    3. 1 2 3 Santos-Sanz, P., Lellouch, E., Fornasier, S., Kiss, C., Pal, A., Müller, T. G., Vilenius, E., Stansberry, J., Mommert, M., Delsanti, A., Mueller, M., Peixinho, N., Henry, F., Ortiz, J. L., Thirouin, A., Protopapa, S., Duffard, R., Szalai, N., Lim, T., Ejeta, C., Hartogh, P., Harris, A. W., & Rengel, M. (2012). “TNOs are Cool”: A Survey of the Transneptunian Region IV - Size/albedo characterization of 15 scattered disk and detached objects observed with Herschel Space Observatory-PACS arXiv:1202.1481
    4. 1 2 3 4 Muller, T.G.; Lellouch, E.; Stansberry, J.; et al. (2010). ""TNOs are Cool": A survey of the trans-Neptunian region I. Results from the Herschel science demonstration phase (SDP)". Astronomy and Astrophysics. 518: L146. arXiv: 1005.2923 . Bibcode:2010A&A...518L.146M. doi:10.1051/0004-6361/201014683. S2CID   118635387.
    5. 1 2 Sheppard, Scott S. (2010). "The colors of extreme outer Solar System objects". The Astronomical Journal. 139 (4): 1394–1405. arXiv: 1001.3674 . Bibcode:2010AJ....139.1394S. doi:10.1088/0004-6256/139/4/1394. S2CID   53545974.
    6. ↑ Emel’yanenko, V. V; Kiseleva, E. L. (2008). "Resonant motion of trans-Neptunian objects in high-eccentricity orbits". Astronomy Letters. 34 (4): 271–279. Bibcode:2008AstL...34..271E. doi:10.1134/S1063773708040075. S2CID   122634598.
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