A nova (plural novae or novas) is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star, that slowly fades over several weeks or many months. Causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars. All observed novae involve a white dwarf in a close binary system. The main sub-classes of novae are classical novae, recurrent novae (RNe), and dwarf novae. They are all considered to be cataclysmic variable stars.
Classical nova eruptions are the most common type. They are likely created in a close binary star system consisting of a white dwarf and either a main sequence, subgiant, or red giant star. When the orbital period falls in the range of several days to one day, the white dwarf is close enough to its companion star to start drawing accreted matter onto the surface of the white dwarf, which creates a dense but shallow atmosphere. This atmosphere, mostly consisting of hydrogen, is thermally heated by the hot white dwarf and eventually reaches a critical temperature causing ignition of rapid runaway fusion.
The sudden increase in energy expels the atmosphere into interstellar space creating the envelope seen as visible light during the nova event and in past centuries mistaken as a "new" star. A few novae produce short-lived nova remnants, lasting for perhaps several centuries. Recurrent nova processes are the same as the classical nova, except that the fusion ignition may be repetitive because the companion star can again feed the dense atmosphere of the white dwarf.
Novae most often occur in the sky along the path of the Milky Way, especially near the observed galactic centre in Sagittarius; however, they can appear anywhere in the sky. They occur far more frequently than galactic supernovae, averaging about ten per year. Most are found telescopically, perhaps only one every 12–18 months reaching naked-eye visibility. Novae reaching first or second magnitude occur only several times per century. The last bright nova was V1369 Centauri reaching 3.3 magnitude on 14 December 2013.[1]
Etymology
During the sixteenth century, astronomer Tycho Brahe observed the supernova SN 1572 in the constellation Cassiopeia. He described it in his book De nova stella (Latin for "concerning the new star"), giving rise to the adoption of 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. Although this event was a supernova and not a nova, the terms were considered interchangeable until the 1930s.[2] After this, novae were classified as classical novae to distinguish them from supernovae, as their causes and energies were thought to be different, based solely in the observational evidence.
Although the term "stella nova" means "new star", novae most often take place as a result of white dwarfs, which are remnants of extremely old stars.
Stellar evolution of novae
Nova Eridani 2009 (apparent magnitude ~8.4)
Evolution of potential novae begins with two main sequence stars in a binary system. One of the two evolves into a red giant, leaving its remnant white dwarf core in orbit with the remaining star. The second star—which may be either a main sequence star or an aging giant—begins to shed its envelope onto its white dwarf companion when it overflows its Roche lobe. As a result, the white dwarf steadily captures matter from the companion's outer atmosphere in an accretion disk, and in turn, the accreted matter falls into the atmosphere. As the white dwarf consists of degenerate matter, the accreted hydrogen does not inflate, but its temperature increases. Runaway fusion occurs when the temperature of this atmospheric layer reaches ~20 million K, initiating nuclear burning, via the CNO cycle.[3]
Hydrogen fusion may occur in a stable manner on the surface of the white dwarf for a narrow range of accretion rates, giving rise to a super soft X-ray source, but for most binary system parameters, the hydrogen burning is unstable thermally and rapidly converts a large amount of the hydrogen into other, heavier chemical elements in a runaway reaction,[2] liberating an enormous amount of energy. This blows the remaining gases away from the surface of the white dwarf surface and produces an extremely bright outburst of light.
The rise to peak brightness may be very rapid, or gradual. This is related to the speed class of the nova; yet after the peak, the brightness declines steadily.[4] The time taken for a nova to decay by around 2 or 3 magnitudes from maximum optical brightness is used for classification, via its speed class. Fast novae typically will take fewer than 25 days to decay by 2 magnitudes, while slow novae will take more than 80 days.[5]
In spite of their violence, usually the amount of material ejected in novae is only about 1⁄10,000 of a solar mass, quite small relative to the mass of the white dwarf. Furthermore, only five percent of the accreted mass is fused during the power outburst.[2] 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.[2][6] In 2010 scientists using NASA's Fermi Gamma-ray Space Telescope discovered that a nova also can emit gamma-rays (>100 MeV).[7]
Potentially, a white dwarf can 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 2006). Eventually, the white dwarf could explode as a Type Ia supernova if it approaches the Chandrasekhar limit.
Occasionally, novae are bright enough and close enough to Earth 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 were V1280 Scorpii, which reached magnitude 3.7 on 17 February 2007, and Nova Delphini 2013. Nova Centauri 2013 was discovered 2 December 2013 and so far, is the brightest nova of this millennium, reaching magnitude 3.3.
Helium novae
A helium nova (undergoing a helium flash) is a proposed category of nova events that lacks hydrogen lines in its spectrum. This may be caused by the explosion of a helium shell on a white dwarf. The theory was first proposed in 1989, and the first candidate helium nova to be observed was V445 Puppis in 2000.[8] Since then, four other novae have been proposed as helium novae.[9]
Occurrence rate and astrophysical significance
Astronomers estimate that the Milky Way experiences roughly 30 to 60 novae per year, but a recent examination has found the likely improved rate of about 50±27.[10] The number of novae discovered in the Milky Way each year is much lower, about 10,[11] probably due to distant novae being obscured by gas and dust absorption.[11] Roughly 25 novae brighter than about the twentieth magnitude are discovered in the Andromeda Galaxy each year and smaller numbers are seen in other nearby galaxies.[12] As of 2019, 407 probable novae are recorded in the Milky Way.[11]
Spectroscopic observation of nova ejecta nebulae has shown that they are enriched in elements such as helium, carbon, nitrogen, oxygen, neon, and magnesium.[2] The contribution of novae to the interstellar medium is not great; novae supply only 1⁄50 as much material to the Galaxy as do supernovae, and only 1⁄200 as much as red giant and supergiant stars.[2]
Recurrent novae such as 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.[13] The recurrence interval for a nova is less dependent on the accretion rate of the white dwarf, than on its mass; with their powerful gravity, massive white dwarfs require less accretion to fuel an eruption than lower-mass ones.[2] Consequently, the interval is shorter for high-mass white dwarfs.[2]
V Sagittae is unusual in that we can predict now that it will go nova in approximately 2083, plus or minus about 11 years.[14]
On 27 May 2020, astronomers reported that classical novae explosions are the galactic producers of the element lithium.[15][16]
Subtypes
Novae are classified according to the light curve development speed, so in
NA: fast novae, with a rapid brightness increase, followed by a brightness decline of 3 magnitudes — to about 1⁄16 brightness — within 100 days.[17]
NB: slow novae, with magnitudes of 3, decline in 150 days or more.
NC: very slow novae, also known as symbiotic novae, staying at maximum light for a decade or more and then fading very slowly.
NR/RN: recurrent novae, novae with two or more eruptions separated by 10–80 years have been observed.[18]
Remnants
GK Persei: Nova of 1901
Main article: Nova remnant
Some novae leave behind visible nebulosity, material expelled in the nova explosion or in multiple explosions. [19]
Novae as distance indicators
Novae have some promise for use as standard candle measurements of distances. 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 measured with Cepheid variable stars, have shown them to be of comparable accuracy.[20]
Recurrent novae
Recurrent novae (RNe) are objects that have been seen to experience multiple nova eruptions. As of 2009, there are ten known galactic recurrent novae,[21] as well as several extragalactic ones (in the Andromeda Galaxy (M31) and the Large Magellanic Cloud). One of these extragalactic novae, M31N 2008-12a, erupts as frequently as once every 12 months. The recurrent nova typically brightens by about 8.6 magnitudes, whereas a classic nova may brighten by more than 12 magnitudes.[21] The ten known galactic recurrent novae are listed below.
Full name
Discoverer
Magnitude
range
Days to drop
3 magnitudes
from peak Known eruption years Time span (years) Years since latest eruption
CI Aquilae K. Reinmuth 8.6–16.3 40 2000, 1941, 1917 24–59 20
V394 Coronae Australis L. E. Erro 7.2–19.7 6 1987, 1949 38 33
T Coronae Borealis J. Birmingham 2.5–10.8 6 1946, 1866 80 74
IM Normae I. E. Woods 8.5–18.5 70 2002, 1920 ≤82 18
RS Ophiuchi W. Fleming 4.8–11 14 2006, 1985, 1967, 1958, 1933, 1898 9–35 14
V2487 Ophiuchi K. Takamizawa (1998) 9.5–17.5 9 1998, 1900 98 22
T Pyxidis H. Leavitt 6.4–15.5 62 2011, 1967, 1944, 1920, 1902, 1890 12–44 9
V3890 Sagittarii H. Dinerstein 8.1–18.4 14 2019, 1990, 1962 28–29 1
U Scorpii N. R. Pogson 7.5–17.6 2.6 2010, 1999, 1987, 1979, 1936, 1917, 1906, 1863 8–43 10
V745 Scorpii L. Plaut 9.4–19.3 7 2014, 1989, 1937 25–52 6
Extragalactic novae
Nova in Andromeda Galaxy
Novae are relatively common in the Andromeda Galaxy (M31).[12] Approximately several dozen novae (brighter than about apparent magnitude 20) are discovered in M31 each year.[12] The Central Bureau for Astronomical Telegrams (CBAT) tracked novae in M31, M33, and M81.[22]
See also
Cosmic distance ladder
Crab Nebula
Guest star (astronomy)
Superluminous supernova
Supernova
Supernova impostor
X-ray burster
References
"Nova Centauri 2013: Another bright, naked-eye nova | aavso.org". www.aavso.org. Retrieved 2 November 2020.
Prialnik, Dina (2001). "Novae". In Paul Murdin (ed.). Encyclopedia of Astronomy and Astrophysics. Institute of Physics Publishing/Nature Publishing Group. pp. 1846–1856. ISBN 978-1-56159-268-5.
M.J. Darnley; et al. (10 February 2012). "On the Progenitors of Galactic Novae". The Astrophysical Journal. 746 (61): 61. arXiv:1112.2589. Bibcode:2012ApJ...746...61D. doi:10.1088/0004-637x/746/1/61. S2CID 119291027.
AAVSO Variable Star Of The Month: May 2001: Novae
Warner, Brian (1995). Cataclysmic Variable Stars. Cambridge University Press. ISBN 978-0-521-41231-5.
Zeilik, Michael (1993). Conceptual Astronomy. John Wiley & Sons. ISBN 978-0-471-50996-7.
JPL/NASA (12 August 2010). "Fermi detects 'shocking' surprise from supernova's little cousin". PhysOrg. Retrieved 15 August 2010.
Kato, Mariko; Hachisu, Izumi (December 2005). "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. S2CID 17055772.
Rosenbush, A. E. (17–21 September 2007). Klaus Werner; Thomas Rauch (eds.). "List of Helium Novae". Hydrogen-Deficient Stars. Eberhard Karls University, Tübingen, Germany (published July 2008). 391: 271. Bibcode:2008ASPC..391..271R.
Shafter, A.W. (January 2017). "The Galactic Nova Rate Revisited". The Astrophysical Journal. 834 (2): 192–203. arXiv:1606.02358. Bibcode:2017ApJ...834..196S. doi:10.3847/1538-4357/834/2/196. S2CID 118652484.
"CBAT List of Novae in the Milky Way". IAU Central Bureau for Astronomical Telegrams.
"M31 (Apparent) Novae Page". IAU Central Bureau for Astronomical Telegrams. Retrieved 24 February 2009.
Seeds, Michael A. (1998). Horizons: Exploring the Universe (5th ed.). Wadsworth Publishing Company. p. 194. ISBN 978-0-534-52434-0.
"Binary star V Sagittae to explode as very bright nova by century's end". phys.org. Retrieved 20 January 2020.
Arizona State University (1 June 2020). "Class of stellar explosions found to be galactic producers of lithium". EurekAlert!. Retrieved 2 June 2020.
Starrfield, Sumner; et al. (27 May 2020). "Carbon–Oxygen Classical Novae Are Galactic 7Li Producers as well as Potential Supernova Ia Progenitors". The Astrophysical Journal. 895 (1): 70. arXiv:1910.00575. Bibcode:2020ApJ...895...70S. doi:10.3847/1538-4357/ab8d23. S2CID 203610207.
"Ritter Cataclysmic Binaries Catalog (7th Edition, Rev. 7.13)". High Energy Astrophysics Science Archive Research Center. 31 March 2010. Retrieved 25 September 2010.
GCVS' vartype.txt at VizieR
Liimets, T.; Corradi, R.L.M.; Santander-García, M.; Villaver, E.; Rodríguez-Gil, P.; Verro, K.; Kolka, I. (2014). "A Dynamical Study of the Nova Remnant of GK Persei / Stella Novae: Past and Future Decades.". Stellar Novae: Past and Future Decades. ASP Conference Series. 490. pp. 109–115. arXiv:1310.4488. Bibcode:2014ASPC..490..109L.
Robert, Gilmozzi; Della Valle, Massimo (2003). "Novae as Distance Indicators". In Alloin, D.; Gieren, W. (eds.). Stellar Candles for the Extragalactic Distance Scale. Springer. pp. 229–241. ISBN 978-3-540-20128-1.
Schaefer, Bradley E. (2010). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". The Astrophysical Journal Supplement Series. 187 (2): 275–373. arXiv:0912.4426. Bibcode:2010ApJS..187..275S. doi:10.1088/0067-0049/187/2/275. S2CID 119294221.
Bishop, David. "Extragalactic Novae". International Supernovae Network. Retrieved 11 September 2010.
Further reading
Payne-Gaposchkin, C. (1957). The Galactic Novae. North Holland Publishing Co.
Hernanz, M.; Josè, J. (2002). Classical Nova Explosions. American Institute of Physics.
Bode, M.F.; Evans, E. (2008). Classical Novae. Cambridge University Press.
External links
Schaefer (2010). "Comprehensive Photometric Histories of All Known Galactic Recurrent Novae". The Astrophysical Journal Supplement Series. 187 (2): 275–373. arXiv:0912.4426. Bibcode:2010ApJS..187..275S. doi:10.1088/0067-0049/187/2/275. S2CID 119294221.
Shafter; et al. (2011). "A Spectroscopic and Photometric Survey of Novae in M31". The Astrophysical Journal. 734 (1): 12. arXiv:1104.0222. Bibcode:2011ApJ...734...12S. doi:10.1088/0004-637X/734/1/12. S2CID 119114867.
General Catalog of Variable Stars, Sternberg Astronomical Institute, Moscow
AAVSO Variable Star of the Month. Novae: May 2001
Extragalactic Novae
vte
Novae
Recurrent novae
T Coronae Borealis IM Normae RS Ophiuchi T Pyxidis U Scorpii
Classical novae
CK Vulpeculae (1670) T Scorpii (1860) T Aurigae (1891) Nova Sagittarii 1898 (1898) V606 Aquilae (1899) GK Persei (1901) DM Geminorum (1903) V604 Aquilae (1905) DI Lacertae (1910) DN Geminorum (1912) V603 Aquilae (1918) HR Lyrae (1919) V849 Ophiuchi (1919) V476 Cygni (1920) RR Pictoris (1925) XX Tauri (1927) DQ Herculis (1934) CP Lacertae (1936) BT Monocerotis (1939) CP Puppis (1942) V500 Aquilae (1943) CT Serpentis (1948) DK Lacertae (1950) RW Ursae Minoris (1956) V446 Herculis (1960) V533 Herculis (1963) HR Delphini (1967) FH Serpentis (1970) V1500 Cygni (1975) V373 Scuti (1975) NQ Vulpeculae (1976) V1668 Cygni (1978) QU Vulpeculae (1984) V842 Centauri (1986) V838 Herculis (1991) V1974 Cygni (1992) V382 Velorum (1999) V1494 Aquilae (1999) V445 Puppis (2000) V598 Puppis (2007) V1280 Scorpii (2007) KT Eridani (2009) V339 Delphini (2013) V1369 Centauri (2013) V5856 Sagittarii (2016)
See also: List of novae in the Milky Way galaxy
vte
Supernovae
Classes
Type Ia Type Ib and Ic Type II (IIP, IIL, IIn, and IIb) Hypernova Superluminous Pair-instability
Physics of
Calcium-rich Carbon detonation Foe Near-Earth Phillips relationship Nucleosynthesis
P-process R-process Neutrinos
Related
Imposter
pulsational pair-instability Failed Gamma-ray burst Kilonova Luminous red nova Nova Pulsar kick Quark-nova Symbiotic nova
Progenitors
Hypergiant
yellow Luminous blue variable Supergiant
blue red yellow White dwarf
related links Wolf–Rayet star
Remnants
Supernova remnant
Pulsar wind nebula Neutron star
pulsar magnetar related links Stellar black hole
related links Compact star
quark star exotic star Zombie star Local Bubble Superbubble
Orion–Eridanus
Discovery
Guest star History of supernova observation Timeline of white dwarfs, neutron stars, and supernovae
Lists
Candidates Notable Massive stars Most distant Remnants In fiction
Notable
Barnard's Loop Cassiopeia A Crab
Crab Nebula iPTF14hls Tycho's Kepler's SN 1987A SN 185 SN 1006 SN 2003fg Remnant G1.9+0.3 SN 2007bi SN 2011fe SN 2014J SN Refsdal Vela Remnant
Research
ASAS-SN Calán/Tololo Survey High-Z Supernova Search Team Katzman Automatic Imaging Telescope Monte Agliale Supernovae and Asteroid Survey Nearby Supernova Factory Sloan Supernova Survey Supernova/Acceleration Probe Supernova Cosmology Project SuperNova Early Warning System Supernova Legacy Survey Texas Supernova Search
vte
White dwarf
Formation
Chandrasekhar limit PG 1159 star Stellar evolution Hertzsprung–Russell diagram Mira variable
Fate
Black dwarf Type Ia supernova
Candidates Neutron star
Pulsar Magnetar Related links Stellar black hole
Related links Compact star
Quark star Exotic star Extreme helium star Subdwarf B star Helium planet
In binary
systems
Nova
Remnant List Dwarf nova Symbiotic nova Cataclysmic variable star
AM CVn star Polar Intermediate polar X-ray binary
Super soft X-ray source Binary pulsar
X-ray pulsar List Helium flash Carbon detonation
Properties
Pulsating Urca process Electron-degenerate matter Quasi-periodic oscillations
Related
Planetary nebula
List RAMBOs White dwarf luminosity function Timeline of white dwarfs, neutron stars, and supernovae
List-Class article List Category Category Commons page WikiCommons
vte
Variable stars
Pulsating
Cepheids and
cepheid-like
Type I (Classical cepheids, Delta Scuti) Type II (BL Herculis, W Virginis, RV Tauri) RR Lyrae Rapidly oscillating Ap SX Phoenicis
Blue-white with
early spectra
Alpha Cygni Beta Cephei Slowly pulsating B-type PV Telescopii Blue large-amplitude pulsator
Long-period
Mira Semiregular Slow irregular
Other
Gamma Doradus Solar-like oscillations White dwarf
Eruptive
Protostar and PMS
Herbig Ae/Be Orion
FU Orionis T Tauri
Giants and
supergiants
Luminous blue variable R Coronae Borealis (DY Persei) Yellow hypergiant
Eruptive binary
Double periodic FS Canis Majoris RS Canum Venaticorum
Other
Flare Gamma Cassiopeiae Lambda Eridani Wolf–Rayet
Cataclysmic
AM Canum Venaticorum Dwarf nova Luminous red nova Nova Polar Intermediate polar Supernova
Hypernova SW Sextantis Symbiotic
Symbiotic nova Z Andromedae
Rotating
Non-spherical
Rotating ellipsoidal
Stellar spots
BY Draconis FK Comae Berenices
Magnetic fields
Alpha² Canum Venaticorum Pulsar SX Arietis
Eclipsing
Algol Beta Lyrae Planetary transit W Ursae Majoris
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