V407 Lupi

From WikiProjectMed
Jump to navigation Jump to search
V407 Lupi
Location of V407 Lupi (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Lupus
Right ascension 15h 29m 01.820s[1]
Declination −44° 49′ 40.89″[1]
Apparent magnitude (V) 5.6 – 14.8 [2]
Characteristics
Variable type Nova[3]
Other designations
Nova Lupi 2016, V407 Lup, PNV J15290182-4449409, ASASSN -16kt[4]
Database references
SIMBADdata
The light curve of V407 Lupi, plotted from AAVSO data

V407 Lupi, also known as Nova Lupi 2016, was a bright nova in the constellation Lupus discovered by All Sky Automated Survey for SuperNovae (ASAS-SN) on 24.00 September 2016. At the time of its discovery, it had an apparent visual magnitude of 9.1. The ASAS-SN team reported that no object at the nova's location brighter than magnitude 17.5 was seen on images taken four days earlier.[5] Wildly incorrect coordinates (in error by many degrees) were published in the announcement telegram,[5] but corrected in a subsequent telegram.[1] It reached a peak brightness of magnitude 5.6, faintly visible to the naked eye, on 25 September 2016.[6] [7]

V407 Lupi declined from its peak brightness very quickly, fading by 2 magnitudes in less than three days. That is one of the most rapid declines in brightness ever seen in a nova. It is therefore classified as a "very fast" nova in the classification scheme of Cecilia Payne-Gaposchkin.[7][8]

All novae are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close to each other that matter is transferred from the donor to the white dwarf. Observations by the satellite TESS detected a variation in the light curve of V407 Lupi indicating an orbital period for the binary system of 3.513 days;[9] it was previously thought to be 3.573 hours,[10] but this has since been disproven.[9] A second periodicity in the light curve was also detected by the Chandra X-ray Observatory[7] and has a period of 591.27465 seconds (9.8545775 min), which appears to be the rotation period of the white dwarf.[9][11] The very rapid decline from peak brightness indicates that the mass of the white dwarf is ≥ 1.25 M☉, not far below the Chandrasekhar limit for white dwarf masses. The system is probably an intermediate polar nova.[7]

References

  1. ^ a b c Stanek, K.Z.; Team, ASAS-SN (September 2016). "Erratum to ATel 9538: ASAS-SN Discovery of A Likely Galactic Nova ASASSN-16kt at V=9.1". The Astronomer's Telegram. 9539: 1. Bibcode:2016ATel.9539....1S. Retrieved 10 January 2021.
  2. ^ "Download Data". aavso.org. AAVSO. Retrieved 9 January 2021.
  3. ^ Izzo, L.; Cano, Z.; de Ugarte Postigo, A.; Thoene, C.; Vanzi, L.; Zapata, A.; Espinoza, N.; Fernandez, D.; Prieto, J.L.; Bonifacio, P.; Della Valle, M.; Molaro, P. (October 2016). "Spectroscopic observations of Nova Lup 2016". The Astronomer's Telegram. 9587: 1. Bibcode:2016ATel.9587....1I. Retrieved 9 January 2021.
  4. ^ "V4407 Lup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-09.
  5. ^ a b Stanek, K.Z.; Kochanek, C.S.; Brown, J.S.; Holoien, T.W.S.; Shields, J.; Shappee, B.J.; Prieto, J.L.; Bersier, D.; Dong, Subo; Bose, S.; Chen, Ping; Chomiuk, L.; Strader, J.; Brimacombe, J. (September 2016). "ASAS-SN Discovery of A Likely Galactic Nova ASASSN-16kt at V=9.1". The Astronomer's Telegram. 9538: 1. Bibcode:2016ATel.9538....1S. Retrieved 11 January 2021.
  6. ^ Watson, Christopher Watson, Christopher. "VSX : Detail for ASASSN-16kt".{{cite web}}: CS1 maint: multiple names: authors list (link)
  7. ^ a b c d Aydi, E.; Orio, M.; Beardmore, A.P.; Ness, J.U.; Page, K.L.; Kuin, N.P.M.; Walter, F.M.; Buckley, D.A.H.; Mohamed, S.; Whitelock, P.; Osborne, J.P.; Strader, J.; Chomiuk, L.; Darnley, M.J.; Dobrotka, A.; Kniazev, A.; Miszalski, B.; Myers, G.; Ospina, N.; Henze, M.; Starrfield, S.; Woodward, C.E. (October 2018). "Multiwavelength observations of V407 Lupi (ASASSN-16kt) - a very fast nova erupting in an intermediate polar". Monthly Notices of the Royal Astronomical Society. 480 (1): 572–609. arXiv:1807.00706. Bibcode:2018MNRAS.480..572A. doi:10.1093/mnras/sty1759. Retrieved 11 January 2021.
  8. ^ Payne-Gaposchkin, Cecilia (1964). The galactic novae. New York: Dover. Bibcode:1964gano.book.....P. Retrieved 11 January 2021.
  9. ^ a b c Schaefer, Bradley E. (2021). "Discovery of 13 New Orbital Periods for Classical Novae". Research Notes of the AAS. 5 (6): 150. arXiv:2106.13907. Bibcode:2021RNAAS...5..150S. doi:10.3847/2515-5172/ac0d5b. S2CID 235632263.
  10. ^ Beardmore, A.P.; Page, K.L.; Osborne, J.P.; Orio, M. (11 August 2021). "Swift observations of nova V407 Lup: detection of a UV period at 1.1 or 3.6 hours". The Astronomer's Telegram. 10632. Retrieved 11 January 2021.
  11. ^ Beardmore, Andy; Dobrotka, Andrej; Ness, Jan-Uwe; Orio, Marina; Osborne, Julian; Page, Kim (September 2017). "Detection of a 9.4 min periodicity in the XMM-Newton and Chandra X-ray light curves of V407 Lup (Nova Lup 2016)". The Astronomer's Telegram. 10749: 1. Bibcode:2017ATel10749....1B. Retrieved 11 January 2021.
Stub icon

This variable star–related article is a stub. You can help Wikipedia by expanding it.

Retrieved from "https://mdwiki.org/wiki/V407_Lupi"