Artist's conception of a white dwarf star accreting hydrogen from a larger companion

A nova (plural novae) is a cataclysmic nuclear explosion in a star caused by the accretion of hydrogen on to the surface of a white dwarf star, which ignites and starts nuclear fusion in a runaway manner. Novae are not to be confused with supernovae or luminous red novae.



If a white dwarf has a close companion star that overflows its Roche lobe, the white dwarf will steadily accrete gas from the companion's outer atmosphere. The companion may be a main sequence star, or one that is aging and expanding into a red giant. The captured gases consist primarily of hydrogen and helium, the two principal constituents of ordinary matter in the universe. The gases are compacted on the white dwarf's surface by its intense gravity, compressed and heated to very high temperatures as additional material is drawn in. The white dwarf consists of degenerate matter, and so does not inflate at increased heat, while the accreted hydrogen is compressed upon the surface. The dependence of the hydrogen fusion rate on temperature and pressure means that it is only when it is compressed and heated at the surface of the white dwarf to a temperature of some 20 million kelvin that a nuclear fusion reaction occurs; at these temperatures, hydrogen burns via the CNO cycle.

For most binary system parameters, the hydrogen burning is thermally unstable and rapidly converts a large amount of the hydrogen into other heavier elements in a runaway reaction.[1] (Hydrogen fusion can occur in a stable manner on the surface, but only for a narrow range of accretion rates.) The enormous amount of energy liberated by this process blows the remaining gases away from the white dwarf's surface and produces an extremely bright outburst of light. The rise to peak brightness can be very rapid or gradual which is related to the speed class of the nova; after the peak, the brightness declines steadily.[2] The time taken for a nova to decay by 2 or 3 magnitudes from maximum optical brightness is used to classify a nova via its speed class. A fast nova will typically take less than 25 days to decay by 2 magnitudes and a slow nova will take over 80 days.[3]

In spite of their violence, the amount of material ejected in novae is usually only about 110,000 of a solar mass, quite small relative to the mass of the white dwarf. Furthermore, only five percent of the accreted mass is fused to power the outburst.[1] Nonetheless, this is enough energy to accelerate nova ejecta to velocities as high as several thousand kilometers per second—higher for fast novae than slow ones—with a concurrent rise in luminosity from a few times solar to 50,000–100,000 times solar.[1][4] In 2010 scientists using NASA's Fermi Gamma-ray Space Telescope were surprised to discover, for the first time, that a nova can also emit gamma-rays (>100 MeV).[5]

A helium nova is a proposed category of nova explosion that lacks hydrogen lines in the spectrum. This may be caused by the explosion of a helium shell on a white dwarf. It was proposed by Kato, Saio and Hachisu in 1989. The first candidate helium nova to be observed was V445 Puppis in 2000.[6] Since then, four other novae explosions have been proposed as helium novae.[7]

A white dwarf can potentially generate multiple novae over time as additional hydrogen continues to accrete onto its surface from its companion star. An example is RS Ophiuchi, which is known to have flared six times (in 1898, 1933, 1958, 1967, 1985, and again in 2006). Eventually, the white dwarf could explode as a type Ia supernova if it exceeds the Chandrasekhar limit.

Occasionally a nova is bright enough and close enough to be conspicuous to the unaided eye. The brightest recent example was Nova Cygni 1975. This nova appeared on 29 August 1975, in the constellation Cygnus about five degrees north of Deneb and reached magnitude 2.0 (nearly as bright as Deneb). The most recent was V1280 Scorpii which reached magnitude 3.7 on 17 February 2007.

Occurrence rate, and astrophysical significance

Astronomers estimate that the Milky Way experiences roughly 30 to 60 novae per year, with a likely rate of about 40.[1] The number of novae discovered in the Milky Way each year is much lower, about 10.[8] Roughly 25 novae brighter than about magnitude 20 are discovered in the Andromeda Galaxy each year and smaller numbers are seen in other nearby galaxies.[9]

Spectroscopic observation of nova ejecta nebulae has shown that they are enriched in elements such as helium, carbon, nitrogen, oxygen, neon and magnesium.[1] The contribution of novae to the interstellar medium is not great; novae supply only 150 as much material to the Galaxy as supernovae, and only 1200 as much as red giant and supergiant stars.[1]

Recurrent novae like RS Ophiuchi (those with periods on the order of decades) are rare. Astronomers theorize however that most, if not all, novae are recurrent, albeit on time scales ranging from 1,000 to 100,000 years.[10] The recurrence interval for a nova is less dependent on the white dwarf's accretion rate than on its mass; with their powerful gravity, massive white dwarfs require less accretion to fuel an outburst than lower-mass ones.[1] Consequently, the interval is shorter for high-mass white dwarfs.[1]


Novae are classified according to the light curve development speed, thus in

  • NA: Fast novae, with a rapid brightness increase, followed by a brightness decline of 3 magnitudes — to circa 116 brightness — within 100 days.[11]
  • NB: Slow novae, with a 3 magnitudes decline in 150 days or more.
  • NC: Very slow novae, staying at maximum light for a decade or more, fading very slowly. It is possible that NC type novae are objects differing physically very much from normal novae, for example planetary nebulae in formation. Exhibiting Wolf-Rayet star like features.
  • NR/RN: Recurrent novae, novae with two or more outbursts (instead of a single one) separated by 10–80 years have been observed.[12]


The astronomer Tycho Brahe observed the supernova SN 1572 in the constellation Cassiopeia, and described it in his book de stella nova (Latin for "concerning the new star"), giving rise to the name nova. In this work he argued that a nearby object should be seen to move relative to the fixed stars, and that the nova had to be very far away. Though this was a supernova and not a classical nova, the terms were considered interchangeable until the 1930s.[1]

Novae as distance indicators

Nova Eridani 2009 (apparent magnitude ~8.4) during a full moon

Novae have some promise for use as standard candles. For instance, the distribution of their absolute magnitude is bimodal, with a main peak at magnitude −8.8, and a lesser one at −7.5. Novae also have roughly the same absolute magnitude 15 days after their peak (−5.5). Comparisons of nova-based distance estimates to various nearby galaxies and galaxy clusters with those done with Cepheid variable stars have shown them to be of comparable accuracy.[13]

Bright novae since 1890

Over 53 novae have been registered since 1890.

Recurrent novae

There are ten known galactic recurrent novae.[14] The recurrent nova typically brightens by about 8.6 magnitude, whereas a classic nova brightens by more than 12 magnitude.[14] Some of the better known and more easily observed recurrent novae are listed below.

Full name
Short name
Days to drop
3 magnitude
from peak
Eruption years
RS Ophiuchi RS Oph 4.8–11 14 2006, 1985, 1967, 1958
T Coronae Borealis T CrB 2.5–10.8 6 1946, 1866
T Pyxidis T Pyx 6.4–15.5 62 2011, 1967, 1944, 1920, 1902
U Scorpii U Sco 7.5–17.6 2.6 2010, 1999, 1987, 1979

Extragalactic novae

Novae in M31 are relatively common.[9] There are roughly a couple dozen novae to be discovered (brighter than about apparent magnitude 20) in M31 each year.[9] The Central Bureau for Astronomical Telegrams (CBAT) tracks novae in M31, M33, and M81.[15]

See also


  1. ^ a b c d e f g h i Prialnik, Dina (2001). "Novae". In Paul Murdin. Encyclopedia of Astronomy and Astrophysics. Institute of Physics Publishing/Nature Publishing Group. pp. 1846–1856. ISBN 1-56159-268-4. 
  2. ^ AAVSO Variable Star Of The Month: May 2001: Novae
  3. ^ Warner, Brian (1995). Cataclysmic Variable Stars. Cambridge University Press. ISBN 0521412315. 
  4. ^ Zeilik, Michael (1993). Conceptual Astronomy. John Wiley & Sons. ISBN 0-471-50996-5. 
  5. ^ JPL/NASA (12 August 2010). "Fermi detects 'shocking' surprise from supernova's little cousin". PhysOrg. Retrieved 15 August 2010. 
  6. ^ Kato, Mariko; Hachisu, Izumi (December 2003). "V445 Puppis: Helium Nova on a Massive White Dwarf". The Astrophysical Journal 598 (2): L107–L110. arXiv:astro-ph/0310351. Bibcode 2003ApJ...598L.107K. doi:10.1086/380597. 
  7. ^ Rosenbush, A. E. (September 17–21, 2007). Klaus Werner and Thomas Rauch. ed. List of Helium Novae. Eberhard Karls University, Tübingen, Germany. Bibcode 2008ASPC..391..271R. 
  8. ^ "CBAT List of Novae in the Milky Way". IAU Central Bureau for Astronomical Telegrams. 
  9. ^ a b c "M31 (Apparent) Novae Page". IAU Central Bureau for Astronomical Telegrams. Retrieved 2009-02-24. 
  10. ^ Seeds, Michael A. (1998). Horizons: Exploring the Universe (5th ed.). Wadsworth Publishing Company. p. 194. ISBN 0-534-52434-6. 
  11. ^ "Ritter Cataclysmic Binaries Catalog (7th Edition, Rev. 7.13)". High Energy Astrophysics Science Archive Research Center. 31 March 2010. Retrieved 2010-09-25. 
  12. ^ GCVS' vartype.txt at VizieR
  13. ^ Robert, Gilmozzi; Della Valle, Massimo (2003). "Novae as Distance Indicators". In Alloin, D.; Gieren, W.. Stellar Candles for the Extragalactic Distance Scale. Springer. pp. 229–241. ISBN 3-540-20128-9. 
  14. ^ a b Schaefer, Bradley E. (2009). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". arXiv:0912.4426 [astro-ph.SR]. 
  15. ^ Bishop, David. "Extragalactic Novae". International Supernovae Network. Retrieved 2010-09-11. 

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