V382 Velorum

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1999 Nova seen in the constellation Vela

title: "V382 Velorum" type: doc version: 1 created: 2026-02-28 author: "Wikipedia contributors" status: active scope: public tags: ["novae", "vela-(constellation)", "1999-in-science", "objects-with-variable-star-designations"] description: "1999 Nova seen in the constellation Vela" topic_path: "general/novae" source: "https://en.wikipedia.org/wiki/V382_Velorum" license: "CC BY-SA 4.0" wikipedia_page_id: 0 wikipedia_revision_id: 0

::summary 1999 Nova seen in the constellation Vela ::

| name = V382 Velorum |image=[[Image:V382VelLocation.png|280px]] |caption=Location of V382 Velorum (circled in red) | epoch = J2000.0 | constell = Vela | ra = | dec = | appmag_v = 2.8 Max. 16.6 Min. | class = | b-v = | u-b = | variable = Nova | radial_v = | prop_mo_ra = | prop_mo_dec = | parallax = 0.5599 | p_error = 0.0547 | parallax_footnote = | dist_pc = | absmag_v = | names = | Simbad = V382+Vel

::figure[src="https://upload.wikimedia.org/wikipedia/commons/3/38/V382VelLightCurve.png" caption="The [[light curve]] of V382 Velorum, plotted from [[AAVSO]] data"] ::

V382 Velorum, also known as Nova Velorum 1999, was a bright nova which occurred in 1999 in the southern constellation Vela. V382 Velorum reached a brightness of 2.6 magnitude, making it easily visible to the naked eye. It was discovered by Peter Williams of Heathcote, New South Wales, Australia at 09:30 UT on 22 May 1999. Later that same day it was discovered independently at 10:49 UT by Alan C. Gilmore at Mount John University Observatory in New Zealand.

In its quiescent state, V382 Velorum has a mean visual magnitude of 16.56. It is classified as a fast nova with a smooth light curve.

Like all novae, V382 Velorum is a binary system with two stars orbiting so close to each other that one star, the "donor" star, transfers matter to its companion star which is a white dwarf. The orbital period is 3.5 hours. The white dwarf in this system has a mass of 1.23M⊙. V382 Velorum is a neon nova, a relatively rare type of nova with a O-Ne-Mg white dwarf, rather than the more common C-O white dwarf.

The stars forming V382 Velorum are surrounded by a small emission nebula about 10 arc seconds in diameter.

References

References

  1. [http://iopscience.iop.org/1538-3881/125/3/1507/pdf/1538-3881_125_3_1507.pdf Shore, SN, et al., in The Astronomical Journal, vol. 125, pp. 1507-1518, March 2003]
  2. (May 1999). "Nova Velorum 1999". IAU Circular.
  3. (February 2000). "Nova Velorum 1999=V382 Vel: Astrometry and Photometry". Publications of the Astronomical Society of the Pacific.
  4. (July 2002). "The evolution of Nova V382 Velorum 1999". Astronomy & Astrophysics.
  5. (July 2010). "Catalog of 93 Nova Light Curves: Classification and Properties". The Astronomical Journal.
  6. (May 2006). "The Detection of a 3.5 hr Period in the Classical Nova Velorum 1999 (V382 Vel) and the Long-Term Behavior of the Nova Light Curve". The Astronomical Journal.
  7. (June 2019). "A Light-curve Analysis of 32 Recent Galactic Novae: Distances and White Dwarf Masses". The Astrophysical Journal Supplement Series.
  8. (1 January 2016). "Light-curve Analysis of Neon Novae". The Astrophysical Journal.
  9. (May 2019). "Imaging and Analysis of Neon Nova V382 Vel Shell". Publications of the Astronomical Society of the Pacific.
  10. {{Cite Gaia DR2. 5354475121660180096
  11. (2018). "The distances to Novae as seen by Gaia". Monthly Notices of the Royal Astronomical Society.
  12. "V382 Velorum".

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novaevela-(constellation)1999-in-scienceobjects-with-variable-star-designations