 Comet Oukaimeden imaged by STEREO HI-1B on 26 September 2014 | |
| Discovery | |
|---|---|
| Discovered by | Oukaimeden Observatory 0.5-mreflector (J43)[1] |
| Discovery date | 12 November 2013 |
| Orbital characteristics | |
| Epoch | 20 September 2014[2] |
| Orbit type | Oort cloud |
| Aphelion | ~370,000 AU (6 ly) (inbound)[a] ~680 AU (outbound)[3] |
| Perihelion | 0.62539AU (q)[2] |
| Eccentricity | 0.99868[2] |
| Orbital period | several million years inbound (Barycentric solution forepoch 1950)[3] ~6000years outbound (Barycentric solution for epoch 2050)[3] |
| Inclination | 154.88°[2] |
| Last perihelion | 28 September 2014[2] |
| JupiterMOID | 0.18 AU |
C/2013 V5 (Oukaimeden) is aretrogradeOort cloudcomet discovered on 12 November 2013 byOukaimeden Observatory at anapparent magnitude of 19.4 using a 0.5-meter (20 in)reflecting telescope.[1]
From 5 May 2014 until 18 July 2014 it had anelongation less than 30 degrees from the Sun.[4] By late August 2014 it had brighten toapparent magnitude 8[5] making it a small telescope and high-endbinoculars target for experienced observers. It crossed thecelestial equator on 30 August 2014 becoming aSouthern Hemisphere object.[4] On 16 September 2014 the comet passed 0.480 AU (71,800,000 km; 44,600,000 mi) from Earth.[6] The comet peaked around magnitude 6.2 in mid-September 2014[7][8] but only had anelongation of about 35 degrees from the Sun.[4] On 20 September 2014 the comet was visible inSTEREO HI-1B.[9] The comet came toperihelion (closest approach to the Sun) on 28 September 2014 at a distance of 0.625 AU (93,500,000 km; 58,100,000 mi) from the Sun.[2]
C/2013 V5 is dynamically new. It came from theOort cloud with a loosely bound chaotic orbit that was easily perturbed bygalactic tides andpassing stars. Before entering the planetary region (epoch 1950), C/2013 V5 had an orbital period of several million years.[3] After leaving the planetary region (epoch 2050), it will have an orbital period of about 6000 years.[3]
Theinfrared spectroscopy of the comet revealed that most of its volatile ices, with the exception ofammonia are depleted. Spectrography also revealed that the relative abundance ofethane andmethanol increased in the start of September 2014, suggesting that the ices that comprise the comet are heterogenous.[10]
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