Astronomy:KT Eridani
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Eridanus |
| Right ascension | 04h 47m 54.2015s[1] |
| Declination | −10° 10′ 42.9633″[1] |
| Apparent magnitude (V) | 5.4 Max. 15.0 Min.[2] |
| Characteristics | |
| Variable type | Classical Nova[2] |
| Astrometry | |
| Proper motion (μ) | RA: 6.469±0.053[1] mas/yr Dec.: −11.009±0.052[1] mas/yr |
| Parallax (π) | 0.2044 ± 0.0384[1] mas |
| Distance | 3744+591 −328[2] pc |
| Details | |
| White dwarf | |
| Mass | 1.15-1.25[3] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
KT Eridani (Nova Eridani 2009) was a bright nova in the constellation Eridanus that produced an outburst in 2009. It was the first classical nova ever detected in that constellation.[6] The nova was discovered at 12:52 UT on 25 November 2009 by K. Itagaki at Yamagata, Japan with a 21 cm patrol telescope. At the time of its discovery, it was a magnitude 8.1 object.[7] The discovery occurred after the nova's peak brightness, but the All Sky Automated Survey system had detected the nova on three earlier occasions, allowing a more complete light curve to be produced. The peak magnitude, 5.4, was seen at 15:10 UT on 14 November 2009.[5]
A very high temporal resolution light curve, beginning on 13 November 2009, was obtained from images taken by the Solar Mass Ejection Imager on the Coriolis satellite. These observations show that the peak brightness, magnitude 5.42±0.02, occurred at November 14.67±0.04 UT. The satellite was able to detect the nova until November 27.23±0.04, by which time it had dropped to magnitude 8.3±0.1. It is classified as a very fast nova, meaning it dimmed rapidly after peak brightness.[8]
On 28 December 2009 (44 days after peak brightness) it was detected as a 0.21 milliJansky source at 5 GHz by the Very Large Array. In the following weeks its radio brightness increased and it was detected in additional radio bands.[9] On the other end of the electromagnetic spectrum, the Swift satellite was used to look for X-ray emission from KT Eridani starting on 27 November 2009, and the satellite detected it on 24 December 2009.[10]
In the most common nova systems, the white dwarf accretes matter from a main sequence star. The white dwarf in the KT Eridani system has a mass of between 1.15 and 1.25 M☉.[3] KT Eridani is probably a recurrent nova, although no previous eruption has been observed. It has an orbital period of 𝑃=2.615950±0.00060 days. The companion is probably a subgiant, with a temperature around 6200 K.[11]
See also
- List of novae in the Milky Way galaxy
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Schaefer, Bradley E. (2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society 481 (3): 3033–3051. doi:10.1093/mnras/sty2388. Bibcode: 2018MNRAS.481.3033S.
- ↑ 3.0 3.1 Pei, Songpeng; Orio, Marina; Ness, Jan-Uwe; Ospina, Nataly (2021). "Chandra observations of nova KT Eridani in outburst". Monthly Notices of the Royal Astronomical Society 507 (2): 2073–2086. doi:10.1093/mnras/stab2298.
- ↑ "KT Eridani". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=KT+Eridani.
- ↑ 5.0 5.1 Raj, Ashish; Banerjee, D.P.K.; Ashok, N.M. (August 2013). "Nova KT Eri 2009: Infrared studies of a very fast andsmall amplitude He/N nova". Monthly Notices of the Royal Astronomical Society 433 (2657–2666): 2657–2666. doi:10.1093/mnras/stt946. https://academic.oup.com/mnras/article/433/3/2657/1240188. Retrieved 8 December 2020.
- ↑ Imamura, Kazuyoshi; Tanabe, Kenji (January 2012). "High galactic latitude classical nova KT Eridani: spectroscopic and photometric observational report .". Mem. S.A.It. 83: 820–824. Bibcode: 2012MmSAI..83..820I. http://articles.adsabs.harvard.edu/pdf/2012MmSAI..83..820I. Retrieved 9 December 2020.
- ↑ "Possible Nova in Eridanis". Central Bureau Electronic Telegram 2050: 1. 26 November 2009. http://www.cbat.eps.harvard.edu/iau/cbet/002000/CBET002050.txt. Retrieved 8 December 2020.
- ↑ Hounsell, R.; Bode, M.F.; Hick, P.P.; Buffington, A.; Jackson, B.V.; Clover, J.M.; Shafter, A.W.; Darnley, M.J. et al. (November 2010). "Exquisite Nova Light Curves from the Solar Mass Ejection Imager (SMEI". The Astrophysical Journal 724 (1): 480–486. doi:10.1088/0004-637X/724/1/480. Bibcode: 2010ApJ...724..480H.
- ↑ O'Brien, T.J.; Muxlow, T.W.B.; Stevens, J.; Datta, A.; Roy, N.; Eyres, S.P.S.; Bode, M.F. (11 February 2010). "Radio detections of KT Eri". The Astronomer's Telegram 2434: 1. Bibcode: 2010ATel.2434....1O. http://www.astronomerstelegram.org/?read=2434. Retrieved 9 December 2020.
- ↑ Bode, M.F.; Osborne, J.P.; Page, K.L.; Beardmore, A.P.; Walter, F.M.; Ness, J.U.; Schwarz, G.; Starrfield, S. et al. (January 2010). "Emergence of a Bright and Highly Variable Super-soft Source Phase in Nova KT Eri (2009)". The Astronomer's Telegram 2392: 1. Bibcode: 2010ATel.2392....1B. http://www.astronomerstelegram.org/?read=2392. Retrieved 9 December 2020.
- ↑ Schaefer, Bradley E.; Walter, Frederick M.; Hounsell, Rebekah; Hillman, Yael (2022-10-28). "The Nova KT Eri Is a Recurrent Nova With a Recurrence Time-Scale of 40-50 Years". Monthly Notices of the Royal Astronomical Society 517 (3): 3864–3880. doi:10.1093/mnras/stac2923. ISSN 0035-8711. http://arxiv.org/abs/2210.10448.
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