QU Vulpeculae

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QU Vulpeculae
QUVulLocation.png
Location of QU Vulpeculae (circled in red)
Observation data
Epoch J2000       Equinox J2000
Constellation Vulpecula
Right ascension 20h 26m 46.020s [1]
Declination +27° 50 43.16 [1]
Apparent magnitude  (V)5.3 Max.
17.9 Min. [2]
Astrometry
Proper motion (μ)RA: 1.325±0.509 [1]   mas/yr
Dec.: −3.125±0.522 [1]   mas/yr
Parallax (π)0.7392 ± 0.3657  mas [1]
Distance 1786+3495
−196
[2]   pc
Characteristics
Variable type Classical Nova, eclipsing binary
Other designations
AAVSO 2022+27, Gaia DR2 1860040595206017664 [2] , Nova Vul 1984 b, Nova Vul 2 [3]
Database references
SIMBAD data
The light curve of QU Vulpeculae, plotted from AAVSO data QUVulLightCurve.png
The light curve of QU Vulpeculae, plotted from AAVSO data

QU Vulpeculae, also known as Nova Vulpeculae 1984 Number 2, was the second nova which occurred in 1984 in the constellation Vulpecula (PW Vulpeculae was the first). It was discovered by Peter Collins, an amateur astronomer from Cardiff, California at 22:08 UT on 22 December 1984. At the time of its discovery, the nova's apparent magnitude was 6.8. By the next night, Collins reported its brightness had increased to magnitude 5.6, making it visible to the naked eye. [4]

QU Vulpeculae declined from peak brightness quite rapidly, and had faded by 3 magnitudes in just 40 days, so it is classified as a "fast" nova. [5]

All nova are binary stars, with a "donor" star orbiting a white dwarf. The two stars are so close to each other that material is transferred from the donor to the white dwarf. Since the two stars are separated by a distance comparable to the radius of the donor star, novae are often found to be eclipsing binaries, and QU Vulpeculae shows such eclipses. The eclipses produce a ~0.5 magnitude brightness drop, and they allow the orbital period, 2.68 hours, to be measured. This is an unusual orbital period for a cataclysmic variable star, falling within the "period gap" between 2 and 3 hours. [6]

A few months after the nova eruption, infrared spectroscopy revealed extremely strong emission in the 12.8 micron forbidden transition of singly ionized neon. It was the strongest emission in that spectral transition, relative to the source's continuum, that had ever been observed in an astronomical source. [7] QU Vulpeculae is an ONeMg neon nova, a nova with an oxygen-neon-magnesium white dwarf primary. A neon nova white dwarf is unusually massive, having a mass ≥ 1.2 M, approaching the Chandrasekhar limit. [8] However estimates of current mass of QU Vulpeculae's white dwarf are lower than this, which has led to suggestions that the white dwarf has lost some of its initial mass as a result of the nova outbursts. [9] It is believed that white dwarfs of this type are the remnants of main sequence stars with initial masses of 8 to 12 M. [10]

In the summer of 1985, QU Vulpeculae was detected in all four of the observing bands (1.49, 4.89, 14.94 and 22.46 GHz) available at that time at the Very Large Array. It was the first nova that was imaged shortly after its outburst in the radio regime, and multi-epoch observations showed that the ejecta was expanding. [11]

QU Vulpeculae is surrounded by a nova remnant, a planetary nebula-like shell of the material that was ejected during its outburst. Its remnant appears roughly spherical. [12] In 2020, its radius was measured to be about 2.1 arcseconds, meaning the shell has been expanding at a rate of about 0.058 arcseconds per year. [12]

Related Research Articles

<span class="mw-page-title-main">Nova</span> Nuclear explosion in a white dwarf star

A nova is a transient astronomical event that causes the sudden appearance of a bright, apparently "new" star that slowly fades over weeks or months. All observed novae involve white dwarfs in close binary systems, but causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars. The main sub-classes of novae are classical novae, recurrent novae (RNe), and dwarf novae. They are all considered to be cataclysmic variable stars.

<span class="mw-page-title-main">V1974 Cygni</span> Star in the constellation Cygnus

V1974 Cygni or Nova Cygni 1992 was a nova, visible to the naked eye, in the constellation Cygnus. It was discovered visually with 10×50 binoculars on February 19, 1992, by Peter Collins, an amateur astronomer living in Boulder, Colorado. At that time he first noticed it, it had an apparent magnitude of 7.2. Nine hours later he saw it again, and it had brightened by a full magnitude. For this discovery Collins was awarded the AAVSO Nova Award in 1993. The nova reached magnitude 4.4 at 22:00 UT on 22 February 1992. Images from the Palomar Sky Survey taken before the nova event showed identified a possible precursor which had photographic magnitudes of 18 and 17, but the identification of the precursor is not firm.

<span class="mw-page-title-main">GK Persei</span> Star in the constellation Perseus

GK Persei was a bright nova first observed on Earth in 1901. It was discovered by Thomas David Anderson, an Edinburgh clergyman, at 02:40 UT on 22 February 1901 when it was at magnitude 2.7. It reached a maximum magnitude of 0.2, the brightest nova of modern times until Nova Aquilae 1918. After fading into obscurity at about magnitude 12 to 13 during the early 20th century, GK Persei began displaying infrequent outbursts of 2 to 3 magnitudes. Since about 1980, these outbursts have become quite regular, typically lasting about two months and occurring about every three years. Thus, GK Persei seems to have changed from a classical nova like Nova Aquilae 1918 to something resembling a typical dwarf nova-type cataclysmic variable star.

<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">T Aurigae</span> Nova seen in 1891

T Aurigae was a nova, which lit up in the constellation Auriga in 1891. Thomas David Anderson, an amateur astronomer in Edinburgh, reported that he was "almost certain" he saw the nova at 02:00 UT on 24 January 1892, when it was slightly brighter than χ Aurigae. He mistook the star for 26 Aurigae, although he noted to himself that it seemed brighter than he remembered it being. He saw it twice more during the following week. On 31 January 1892 he realized his mistake, and wrote a note to Ralph Copeland reporting his discovery. Professor Copeland immediately reported the discovery via telegram to William Huggins, who made the first spectroscopic observations of T Aurigae on 2 February 1892, when the star was a magnitude 4.5 object. T Aurigae was the first nova to be observed spectroscopically.

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

DI Lacertae or Nova Lacertae 1910 was a nova in constellation Lacerta which appeared in 1910. It was discovered by Thomas Henry Espinell Compton Espin at Wolsingham Observatory on 30 Dec 1910, at which time it was an 8th magnitude object. Subsequent examination of pre-discovery photographic plates showed that the outburst occurred sometime between 17 November 1910 and 23 November 1910. It reached a peak brightness of magnitude 4.6 on 26 November 1910, making it visible to the naked eye. Before the nova event DI Lacertae was a 14th magnitude star, and by 1950 it had returned to 14th magnitude.

<span class="mw-page-title-main">V446 Herculis</span> 1960 Nova event in the constellation Hercules

V446 Herculis was a nova in the constellation Hercules in 1960. It reached magnitude 2.8. The nova was first observed by Olaf Hassel in the early morning hours of 7 March 1960, when it was a 5th magnitude star. Pre-discovery photographs showed that it was about three days past peak brightness, and had faded by 2 magnitudes during that time. The star was so near the border between the constellations of Hercules and Aquila that accurate measurements of its position were needed to determine which constellation contained it.

<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">V838 Herculis</span> 1991 Nova seen in the constellation Hercules

V838 Herculis, also known as Nova Herculis 1991, was a nova which occurred in the constellation Hercules in 1991. It was discovered by George Alcock of Yaxley, Cambridgeshire, England at 4:35 UT on the morning of 25 March 1991. He found it with 10×50 binoculars, and on that morning its apparent visual magnitude was 5. Palomar Sky Survey plates showed that before the outburst, the star was at photographic magnitude 20.6 and 18.25.

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

V1494 Aquilae or Nova Aquilae 1999 b was a nova which occurred during 1999 in the constellation Aquila and reached a brightness of magnitude 3.9 on 2 December 1999. making it easily visible to the naked eye. The nova was discovered with 14×100 binoculars by Alfredo Pereira of Cabo da Roca, Portugal at 18:50 UT on 1 December 1999, when it had a visual magnitude of 6.0.

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

U Geminorum, in the constellation Gemini, is an archetypal example of a dwarf nova. The binary star system consists of a white dwarf closely orbiting a red dwarf. Every few months it undergoes an outburst that greatly increases its brightness. The dwarf nova class of variable stars are often referred to as U Geminorum variables after this star.

<span class="mw-page-title-main">CK Vulpeculae</span> 1678 Nova seen in the constellation Vulpecula

CK Vulpeculae is an object whose exact nature is unknown. It was once considered to be the oldest reliably-documented nova. It consists of a compact central object surrounded by a bipolar nebula.

<span class="mw-page-title-main">V630 Sagittarii</span> Nova that appeared in 1936

V630 Sagittarii was a nova visible to the naked eye in 1936. It was discovered on 3 October 1936 by Shigeki Okabayashi of Kobe, Japan when it had an apparent magnitude of 4.5.

<span class="mw-page-title-main">LV Vulpeculae</span> Nova seen in 1968 in the constellation Vulpecula

LV Vulpeculae, also known as Nova Vulpeculae 1968 no. 1, was the first of two novae in the constellation of Vulpecula which erupted in 1968. It was discovered by George Alcock who observed it from the back garden of his home in Farcet, England, on the morning of 15 April 1968. The next night it was independently discovered by Midtskoven in Norway. It reached a peak apparent magnitude of 4.79 on 17 April 1968. It was visible to the naked eye at the same time HR Delphini was a naked eye object, and the two novae were less than 15 degrees apart on the sky.

<span class="mw-page-title-main">WY Sagittae</span> 1783 Nova seen in the constellation Sagitta

WY Sagittae, also known as Nova Sagittae 1783, is a star in the constellation Sagitta which had a nova eruption visible in 1783. It was discovered on 26 July 1783 by the French astronomer Joseph Lepaute D'Agelet. It is usually difficult to precisely identify novae that were discovered hundreds of years ago, because the positions were often vaguely reported and historically there was not a clear distinction drawn between different sorts of transient astronomical events such as novae and comet apparitions. However D'Agelet observed this nova with a mural quadrant, which produced coordinates accurate enough to allow modern astronomers to identify the star. D'Agelet reported the apparent magnitude of the star as 6, but Benjamin Apthorp Gould, who analysed D'Agelet's records, determined that what D'Agelet called magnitude 6 corresponds to magnitude 5.4 ± 0.4 on the modern magnitude scale, so the nova was visible to the naked eye.

<span class="mw-page-title-main">V1370 Aquilae</span> Nova that occurred in 1982

V1370 Aquilae, also known as Nova Aquilae 1982, is a nova that appeared in the constellation Aquila during 1982. It was discovered by Minoru Honda of Kurashiki, Japan at 20:30 UT on 27 January 1982. At that time the Sun had moved just far enough from Aquila to allow the nova to be seen in the morning sky. Although it was discovered photographically, its apparent magnitude was 6–7, making it potentially visible to the naked eye under ideal conditions. A possible magnitude 20 progenitor was located on the Palomar Sky Survey prints. Spectra of the object were taken in February 1982 at Asiago Astrophysical Observatory, which confirmed that it is a nova.

<span class="mw-page-title-main">PU Vulpeculae</span> Variable star in the constellation Vulpecula

PU Vulpeculae is a very slowly evolving symbiotic nova in the northern constellation of Vulpecula, abbreviated PU Vul. It is too faint to be visible to the naked eye, reaching a maximum apparent visual magnitude of 8.7 following a minimum of 16.6. The system is located at a distance of approximately 17,000 light years from the Sun based on parallax measurements.

<span class="mw-page-title-main">QQ Vulpeculae</span> Variable star in the constellation Vulpecula

QQ Vulpeculae is a cataclysmic variable binary star system in the northern constellation of Vulpecula, abbreviated QQ Vul. It has a brightness that fluctuates around an apparent visual magnitude of 14.7, which is too faint to be viewed with the naked eye. The distance to this system is approximately 981 light years based on parallax measurements.

<span class="mw-page-title-main">OY Arae</span> 1910 nova in the constellation Ara

OY Arae, also known as Nova Arae 1910, is a nova in the constellation Ara. It was discovered by Williamina Fleming on a Harvard Observatory photographic plate taken on April 4, 1910. At that time it had a magnitude of 6.0, making it faintly visible to the naked eye under ideal observing conditions. Examination of earlier plates showed that before the outburst it was a magnitude 17.5 object, and by March 19, 1910, it had reached magnitude 12.

References

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