CP Lacertae

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CP Lacertae
CPLacLocation.png
Location of CP Lacertae (circled in red)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Lacerta
Right ascension 22h 15m 41.103s [1]
Declination +55° 37 01.44 [1]
Apparent magnitude  (V)2.1 Max.
16.6 Min. [2]
Characteristics
Variable type Nova [2]
Astrometry
Distance 3,800+220
160
  ly
(1170+67
−50
[3]   pc)
Other designations
Nova Lac 1936, AAVSO 2212+55, 2MASS J22154108+5537014 [4]
Database references
SIMBAD data
The light curve of CP Lacertae plotted from AAVSO data CPLacLightCurve.png
The light curve of CP Lacertae plotted from AAVSO data

CP Lacertae (also known as Nova Lacertae 1936 or CP Lac) was a nova, which lit up on June 18, 1936 in the constellation Lacerta. It was discovered independently by several observers including Leslie Peltier in the US, E. Loreta in Italy, and Kazuaki Gomi, a Japanese barber who discovered the nova during the 19 June 1936 total solar eclipse. [5]

The nova reached a peak brightness of 2.1 mag, [6] making it readily visible to the naked eye during night time. Following the outbreak, the brightness of CP Lacertae decreased thereafter, falling 3 magnitudes after nine days. It is classified as a very fast nova, with a smooth light curve. [7] [8]

Located at an estimated distance of 3.8  kly (1.17  kpc ), [3] this is a close binary system with a degenerate white dwarf primary in orbit with a cool red dwarf secondary over a period of 0.145143 days. [9] Matter from the red dwarf is being drawn off onto an accretion disk orbiting the white dwarf. The mean brightness of the system varies with an amplitude of 0.5 magnitude from day to day. The observational data shows a general period of 0.037 days, which may be related to the rotation period of the white dwarf component. [10]

Unlike many novae, CP Lacertae does not have a shell visible as a nebula with optical telescopes. [11]

Related Research Articles

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DQ Herculis, or Nova Herculis 1934, was a slow, bright nova occurring in the northern constellation of Hercules in December 1934. This cataclysmic variable star was discovered on 13 December 1934 by J. P. M. Prentice from Stowmarket, Suffolk. It reached peak brightness on 22 December 1934 with an apparent magnitude of 1.5. The nova remained visible to the naked eye for several months.

<span class="mw-page-title-main">V1500 Cygni</span> Star in the constellation Cygnus

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<span class="mw-page-title-main">V382 Velorum</span> 1999 Nova seen in the constellation Vela

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.

<span class="mw-page-title-main">DI Lacertae</span> 1910 Nova in the constellation Lacerta

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<span class="mw-page-title-main">DN Geminorum</span> Star in the constellation Gemini

DN Geminorum or Nova Geminorum 1912 was a classical nova which lit up in 1912 in the constellation Gemini. It was discovered by Norwegian variable star observer Sigurd Einbu on March 12, 1912 before reaching peak brightness, which allowed early-stage spectra to be collected by Yerkes Observatory. The nova reached a maximum brightness of around 3.5 mag before declining, which means it was visible to the naked eye. Its brightness decreased over the following 36 days by 3 magnitudes as it gradually faded from sight. The light curve saw two maxima a few months after the outburst, along with strong oscillations. Today its brightness is visual magnitude 15.5.

<span class="mw-page-title-main">NQ Vulpeculae</span> 1976 Nova seen in the constellation Vulpecula

NQ Vulpeculae also known as Nova Vulpeculae 1976, was a nova that appeared in the constellation Vulpecula in 1976. It was discovered visually at 18:20 UT on October 21, 1976 by English amateur astronomer George Alcock. Its apparent magnitude at the time of discovery was 6.5 It reached its maximum brightness of magnitude 6.0 thirteen days after its discovery, at which point it may have been faintly visible to the naked eye. A few days after maximum brightness, it had faded to magnitude 8.3.

<span class="mw-page-title-main">DK Lacertae</span> 1950 Nova seen in the constellation Lacerta

DK Lacertae was a nova, which lit up in the constellation Lacerta in 1950. The nova was discovered by Charles Bertaud of the Paris Observatory on a photographic plate taken on 23 January 1950. At the time of its discovery, it had an apparent magnitude of 6.1. DK Lacertae reached peak magnitude 5.0, making it easily visible to the naked eye.

<span class="mw-page-title-main">V1494 Aquilae</span> Nova seen in 1999 in the constellation of Aquila

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Z Camelopardalis (Z Cam) is a cataclysmic variable star system in the northern constellation of Camelopardalis. It has an apparent visual magnitude which varies between 9.8 and 14.5. This system is the prototype star for the family of Z Camelopardalis variable stars: dwarf novae with standstills at a brightness intermediate between their maxima and minima. It may be the same bright nova that was recorded by Chinese astrologers in the autumn of 77 BCE.

<span class="mw-page-title-main">RX Andromedae</span> Cataclysmic variable star system in the constellation Andromeda

RX Andromedae is a variable star in the constellation of Andromeda. Although it is classified as a dwarf nova of the Z Camelopardalis (UGZ) type, it has shown low-luminosity periods typical of VY Sculptoris stars. However, for most of the time it varies from an apparent visual magnitude of 15.1 at minimum brightness to a magnitude of 10.2 at maximum brightness, with a period of approximately 13 days.

<span class="mw-page-title-main">RW Ursae Minoris</span> Nova that appeared in 1956

RW Ursae Minoris is a cataclysmic variable star system that flared up as a nova in the constellation Ursa Minor in 1956.

<span class="mw-page-title-main">HR Delphini</span> 1967 Nova seen in the constellation Delphinus

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<span class="mw-page-title-main">V1017 Sagittarii</span> Star in the constellation Sagittarius

V1017 Sagittarii is a cataclysmic variable star system in the constellation Sagittarius. It first erupted in 1919, reaching magnitude 7. Its other eruptions in 1901, 1973 and 1991 only reached magnitude 10, leading it to be reclassified from a recurrent nova to a dwarf nova.

<span class="mw-page-title-main">IM Normae</span> Recurrent nova in the constellation Norma

IM Normae is a recurrent nova in the constellation Norma, one of only ten known in the Milky Way. It has been observed to erupt in 1920 and 2002, reaching magnitude 8.5 from a baseline of 18.3. It was poorly monitored after the first eruption, so it is possible that it erupted in between these dates.

<span class="mw-page-title-main">16 Lacertae</span> Triple star system in the constellation Lacerta

16 Lacertae is a triple star system in the northern constellation of Lacerta, located about 1,580 light years from the Sun. It has the variable star designation EN Lacertae; 16 Lacertae is the Flamsteed designation. This system is visible to the naked eye as a faint blue-white hued star with a maximum apparent visual magnitude of +5.587. It is moving closer to the Earth with a heliocentric radial velocity of –12 km/s.

<span class="mw-page-title-main">U Lacertae</span> Binary star in the constellation Lacerta

U Lacertae is a spectroscopic binary star in the constellation Lacerta.

<span class="mw-page-title-main">V728 Scorpii</span> Nova seen in 1862

V728 Scorpii, also known as Nova Scorpii 1862, was a nova that occurred in the constellation of Scorpius. It was discovered on 4 October 1862 by John Tebbutt, an astronomer living in New South Wales, Australia, while he was observing a comet. He reported that the star was in the constellation Ara. At the time of its discovery, the nova had an apparent magnitude of 5, making it visible to the unaided eye. Nine days later it had faded to below 11th magnitude, indicating that it was a very fast nova.

<span class="mw-page-title-main">V368 Aquilae</span> Nova seen in 1936

V368 Aquilae, also known as Nova Aquilae 1936 no. 2 was the second nova which occurred in the constellation of Aquila during 1936. It was discovered on a photographic plate by Nils Tamm at Kvistaberg Observatory on 7 October 1936. At the time of discovery it was at photographic magnitude 7, and was already fading. Pre-discovery photographs showed that peak brightness occurred around 25 September 1936, at which time it had reached apparent magnitude 5.0, making it visible to the naked eye. The nova was described as being fiery red due to strong Hα emission, and for a time could be seen with binoculars simultaneously with V356 Aquilae, another nova which Nill Tamm had discovered a month earlier.

<span class="mw-page-title-main">AP Librae</span> Active galactic nucleus in the constellation Libra

AP Librae is a BL Lacertae object located at a distance of 700 million light years in the southern constellation of Libra. In the visual band it is one of the most active blazars known. AP Lib is surrounded by an extended source with a spectrum characteristic of a red-shifted giant elliptical galaxy. The derived visual magnitude of this region is 15.0, and it follows a radially decreasing brightness that is characteristic of an elliptical. Seven fainter galaxies are visible within an angular radius of 9′, suggesting it is the brightest member of a galactic cluster.

References

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  5. Warner, B. (February 2006). "Where have all the novae gone?". Astronomy & Geophysics. 47 (1): 29–32. Bibcode:2006A&G....47a..29W. doi: 10.1111/j.1468-4004.2006.47129.x .
  6. Howarth, I. D. (October 1978), "CP Lacertae (Nova 1936)", Journal of the British Astronomical Association, 88: 608–618, Bibcode:1978JBAA...88..608H.
  7. Rodríguez-Gil, P.; Torres, M.A.P. (February 2005). "Time-resolved photometry of the nova remnants DM Gem, CP Lac, GI Mon, V400 Per, CT Ser and XX Tau" (PDF). Astronomy & Astrophysics. 431: 289–296. arXiv: astro-ph/0410348 . doi: 10.1051/0004-6361:20041112 . Retrieved 6 December 2020.
  8. Tappert, C.; Vogt, N.; Ederoclite, A.; Schmidtobreick, L.; Vuckovic, M.; Becegato, L.L. (September 2020). "The luminosity evolution of nova shells. I. A new analysis of old data". Astronomy & Astrophysics. 641: A122. arXiv: 2007.10940 . Bibcode:2020A&A...641A.122T. doi: 10.1051/0004-6361/202037913 .
  9. Pavlenko, E. P.; et al. (May 2007), "The Photometric Study of Nova Lacertae 1936 = CP Lac Between 2003 – 2005", in Demircan, O.; Selam, S. O.; Albayrak, B. (eds.), Solar and Stellar Physics Through Eclipses ASP Conference Series, Vol. 370, proceedings of the conference held 27–29 March, 2006 at Ankara University, ÖRSEM Campus, Side, Antalya, Turkey, vol. 370, Astronomical Society of the Pacific, p. 324, Bibcode:2007ASPC..370..324P.
  10. Litvinchova, A. A.; Pavlenko, E. P. (December 2010), "The Photometric Investigation of the Active Post-Nova CP Lac in High and Low State of Brightness in 2006–2008 yrs", Odessa Astronomical Publications, 23: 76, Bibcode:2010OAP....23...76L.
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