HD 37836

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HD 37836
Observation data
Epoch J2000       Equinox J2000
Constellation Dorado
Right ascension 5h 35m 16.633s [1]
Declination −69° 40′ 38.44″ [1]
Apparent magnitude  (V)10.55 [2]
Characteristics
Spectral type B0Iae [3]
Apparent magnitude  (U)9.87
Apparent magnitude  (B)10.736
Apparent magnitude  (R)10.73
Apparent magnitude  (I)10.164
Apparent magnitude  (J)9.886
Apparent magnitude  (H)9.72
Apparent magnitude  (K)9.381
Variable type cLBV and α Cygni
Astrometry
Radial velocity (Rv)−474.41 km/s
Parallax (π)0.0271 ± 0.0139  mas [1]
Distance 163,000  ly
(49,970  pc)
Absolute magnitude  (MV)−8.5 [4]
Details
Radius 85 [2]   R☉
Luminosity 4,169,000 [2]   L☉
Surface gravity (log g)2.14 [1]   cgs
Temperature 28,200 [2]   K
Other designations
HD 37836, RMC 123, R123, HIP 26222
Database references
SIMBAD data

HD 37836 is a candidate luminous blue variable located in the Large Magellanic Cloud and one of the brightest stars in its galaxy. [3] [5]

Contents

History

The star was first mentioned in a 1901 paper as an object with an unusual spectrum with bright H-alpha, H-beta and H-delta lines located in the LMC. [6] Later it was catalogued in the Henry Draper Catalogue and given the designation HD 37836. In 1957 it was noted that its spectral lines show a P Cygni profile. [7]

Stellar properties

HD 37836 is an extremely luminous blue supergiant with parameters similar to other similar stars, such as η Carinae A. It is also an α Cygni variable. [8] Its apparent magnitude varies by ~0.2 magnitudes.

In 1983, its luminosity was estimated to be 5.6 million  L☉ and its mass was estimated to be 100 M☉, which would make it one of the most luminous and most massive known stars. [9]

A paper published in 1987 again noted the star's peculiar spectrum. It also concluded that the star might be similar to HD 269445 and Hen S 131. The star's luminosity was estimated to be around 4 million L☉. [10]

A year later, it was classified as a possible S Doradus variable. [11] A 1998 paper considers it an active LBV, an Alpha Cygni variable, and a 2018 census of LBVs considers it to be a candidate. [5] [12]

A 2023 paper estimates its luminosity to be 4.2 million solar luminosities and its temperature to be 28,200 K based on the star's spectral type, corresponding to a radius of 85 solar radii, comparable to that of Rigel. [2]

Related Research Articles

<span class="mw-page-title-main">S Doradus</span> Star in the Large Magellanic Cloud

S Doradus is one of the brightest stars in the Large Magellanic Cloud (LMC), a satellite galaxy of the Milky Way, located roughly 160,000 light-years away. The star is a luminous blue variable, and one of the most luminous stars known, having a luminosity varying widely above and below 1,000,000 times the luminosity of the Sun, although it is too far away to be seen with the naked eye.

<span class="mw-page-title-main">Luminous blue variable</span> Type of star that is luminous, blue, and variable in brightness

Luminous blue variables (LBVs) are massive evolved stars that show unpredictable and sometimes dramatic variations in their spectra and brightness. They are also known as S Doradus variables after S Doradus, one of the brightest stars of the Large Magellanic Cloud. They are extraordinarily rare, with just 20 objects listed in the General Catalogue of Variable Stars as SDor, and a number of these are no longer considered LBVs.

<span class="mw-page-title-main">Yellow hypergiant</span> Class of massive star with a spectral type of A to K

A yellow hypergiant (YHG) is a massive star with an extended atmosphere, a spectral class from A to K, and, starting with an initial mass of about 20–60 solar masses, has lost as much as half that mass. They are amongst the most visually luminous stars, with absolute magnitude (MV) around −9, but also one of the rarest, with just 20 known in the Milky Way and six of those in just a single cluster. They are sometimes referred to as cool hypergiants in comparison with O- and B-type stars, and sometimes as warm hypergiants in comparison with red supergiants.

<span class="mw-page-title-main">HD 37974</span> Star in the constellation Dorado

HD 37974 a variable B[e] hypergiant in the Large Magellanic Cloud. It is surrounded by an unexpected dust disk.

<span class="mw-page-title-main">HR Carinae</span> Star in the constellation Carina

HR Carinae is a luminous blue variable star located in the constellation Carina. It is surrounded by a vast nebula of ejected nuclear-processed material because this star has a multiple shell expanding atmosphere. This star is among the most luminous stars in the Milky Way. It has very broad emission wings on the Balmer lines, reminiscent from the broad lines observed in the spectra of O and Wolf–Rayet stars. A distance of 5 kpc and a bolometric magnitude of -9.4 put HR Car among the most luminous stars of the galaxy.

<span class="mw-page-title-main">WOH G64</span> Star in the constellation Dorado

WOH G64 is an unusual red supergiant (RSG) star in the Large Magellanic Cloud (LMC) satellite galaxy in the southern constellation of Dorado. It is one of the largest known stars, being described as possibly being the largest star known. It is also one of the most luminous and massive red supergiants, with a radius calculated to be around 1,540 times that of the Sun (R☉) and a luminosity around 282,000 times the solar luminosity (L☉).

<span class="mw-page-title-main">Hypergiant</span> Rare star with tremendous luminosity and high rates of mass loss by stellar winds

A hypergiant (luminosity class 0 or Ia+) is a very rare type of star that has an extremely high luminosity, mass, size and mass loss because of its extreme stellar winds. The term hypergiant is defined as luminosity class 0 (zero) in the MKK system. However, this is rarely seen in literature or in published spectral classifications, except for specific well-defined groups such as the yellow hypergiants, RSG (red supergiants), or blue B(e) supergiants with emission spectra. More commonly, hypergiants are classed as Ia-0 or Ia+, but red supergiants are rarely assigned these spectral classifications. Astronomers are interested in these stars because they relate to understanding stellar evolution, especially star formation, stability, and their expected demise as supernovae.

Zeta<sup>1</sup> Scorpii Star in the constellation Scorpius.

Zeta1 Scorpii is a B-type hypergiant star in the constellation of Scorpius. It has an apparent visual magnitude which varies between 4.66 and 4.86. It is a member of the Scorpius OB1 association, and the open star cluster NGC 6231, also known as the "Northern jewel box" cluster. Around 36 times as massive as the Sun, it is also one of the most luminous stars known in the Galaxy, with an estimated bolometric luminosity of around 850,000 times that of the Sun and a radius 103 times that of the Sun.

<span class="mw-page-title-main">HD 33579</span> Star in the constellation Dorado

HD 33579 is a white/yellow hypergiant and one of the brightest stars in the Large Magellanic Cloud (LMC). It is a suspected variable star.

<span class="mw-page-title-main">HD 168607</span> Star in the constellation Sagittarius

HD 168607 is a blue hypergiant and luminous blue variable (LBV) star located in the constellation of Sagittarius, easy to see with amateur telescopes. It forms a pair with HD 168625, also a blue hypergiant and possible luminous blue variable, that can be seen at the south-east of M17, the Omega Nebula.

<span class="mw-page-title-main">HD 160529</span> Luminous blue variable star in the constellation Scorpius

HD 160529 is a luminous blue variable (LBV) star located in the constellation of Scorpius. With an apparent magnitude of around +6.8 cannot be seen with the naked eye except under very favourable conditions, but it is easy to see with binoculars or amateur telescopes.

<span class="mw-page-title-main">V1429 Aquilae</span> Star in the constellation Aquila

V1429 Aquilae is a candidate luminous blue variable multiple star system located in the constellation of Aquila. It is often referred to by its Mount Wilson Observatory catalog number as MWC 314. It is a hot luminous star with strong emission lines in its spectrum.

<span class="mw-page-title-main">AS 314</span> Protoplanetary nebula in the constellation Scutum

AS 314, also known as V452 Scuti, is a protoplanetary nebula once believed to be a white hypergiant star or luminous blue variable located in the constellation of Scutum. It has an apparent magnitude of 9.85 and can be seen with small telescopes.

R99 is a star in the Large Magellanic Cloud in the constellation Dorado. It is classified as a possible luminous blue variable and is one of the most luminous stars known.

<span class="mw-page-title-main">HD 316285</span> Star in the constellation Sagittarius

HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the Galactic Center.

<span class="mw-page-title-main">R85</span> Candidate luminous variable star in the constellation Dorado

R85 is a candidate luminous blue variable located in the LH-41 OB association in the Large Magellanic Cloud.

<span class="mw-page-title-main">R71 (star)</span> Star in the Large Magellanic Cloud

R71 is a star in the Large Magellanic Cloud (LMC) in the constellation Mensa. It is classified as a luminous blue variable and is one of the most luminous stars in the LMC. It lies three arc-minutes southwest of the naked-eye star β Mensae.

<span class="mw-page-title-main">HV 888</span> Star in the constellation Dorado

HV 888, also known as WOH S140, is a red supergiant (RSG) star located in the Large Magellanic Cloud. It is possibly among the largest known stars, with reliable estimates of its radius ranging from 1,353 R☉ to 1,584 R☉, and is also one of the most luminous of its type with a range of nearly 300,000 to over 500,000 times that of the Sun (L☉). The effective temperature is estimated to be around 3,500 K. If placed at the center of the Solar System, its photosphere would engulf the orbit of Jupiter.

<span class="mw-page-title-main">V1936 Aquilae</span> Blue supergiant star in the constellation Aquila

V1936 Aquilae is a blue supergiant and candidate Luminous blue variable located in the nebula Westerhout 51, in the constellation Aquila, about 20,000 light years away. The star was originally identified as a massive star in 2000, and was thought to be an O-type supergiant. However, subsequent analyses have shown it to be not O but B-type, as well as being possibly an LBV.

References

  1. 1 2 3 4 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875.
  2. 1 2 3 4 5 Martin, John C.; Humphreys, Roberta M. (2023-10-30). "A Census of the Most Luminous Stars. I. The Upper HR Diagram for the Large Magellanic Cloud". The Astronomical Journal. 166 (5): 214. Bibcode:2023AJ....166..214M. doi: 10.3847/1538-3881/ad011e . ISSN   0004-6256.
  3. 1 2 Lennon, Daniel J.; Marel, Roeland P. van der; Lerate, Mercedes Ramos; O’Mullane, William; Sahlmann, Johannes (2017-07-01). "Gaia TGAS search for Large Magellanic Cloud runaway supergiant stars - Candidate hypervelocity star discovery and the nature of R 71". Astronomy & Astrophysics. 603: A75. arXiv: 1611.05504 . Bibcode:2017A&A...603A..75L. doi:10.1051/0004-6361/201630076. ISSN   0004-6361. S2CID   119474184.
  4. ↑ Genderen, A. M. van (2001-02-01). "S Doradus variables in the Galaxy and the Magellanic Clouds". Astronomy & Astrophysics. 366 (2): 508–531. Bibcode:2001A&A...366..508V. doi: 10.1051/0004-6361:20000022 . ISSN   0004-6361. S2CID   55796300.
  5. 1 2 Richardson, Noel D.; Mehner, Andrea (2018-07-11). "The 2018 Census of Luminous Blue Variables in the Local Group". Research Notes of the AAS. 2 (3): 121. arXiv: 1807.04262 . Bibcode:2018RNAAS...2..121R. doi: 10.3847/2515-5172/aad1f3 . ISSN   2515-5172.
  6. ↑ Pickering, E. C.; Fleming, W. P. (1901-09-01). "Objects having peculiar spectra" (PDF). The Astrophysical Journal. 14: 144–146. Bibcode:1901ApJ....14..144P. doi:10.1086/140844. ISSN   0004-637X.
  7. ↑ Smith, Henry J. (1957-04-01). "Spectra of Bright-Line Stars in the Large Magellanic Cloud". Publications of the Astronomical Society of the Pacific. 69 (407): 137. Bibcode:1957PASP...69..137S. doi: 10.1086/127032 . ISSN   1538-3873. S2CID   122612430.
  8. ↑ Balona, L A; Handler, G; Chowdhury, S; Ozuyar, D; Engelbrecht, C A; Mirouh, G M; Wade, G A; David-Uraz, A; Cantiello, M (2019-05-21). "Rotational modulation in TESS B stars". Monthly Notices of the Royal Astronomical Society. 485 (3): 3457–3469. arXiv: 1902.09470 . doi: 10.1093/mnras/stz586 . ISSN   0035-8711.
  9. ↑ van Genderen, A. M.; Groot, M.; The, P. S. (1983-01-01). "On the photometric differences between luminous OBA type stars in the LMC with and without P Cygni characteristics". Astronomy and Astrophysics. 117: 53–59. Bibcode:1983A&A...117...53V. ISSN   0004-6361.
  10. ↑ Stahl, O.; Wolf, B. (1987-07-01). "The peculiar emission-line supergiant HD 37836". Astronomy and Astrophysics. 181: 293–299. Bibcode:1987A&A...181..293S. ISSN   0004-6361.
  11. ↑ Lortet, M. C. (1988-12-01). "A provisory catalogue of S-Dor candidate stars in the Magellanic Clouds". Bulletin d'Information du Centre de Donnees Stellaires. 35: 145–154. Bibcode:1988BICDS..35..145L. ISSN   1169-8837.
  12. ↑ van Genderen, A. M.; Sterken, C.; de Groot, M.; Reijns, R. A. (1998-04-01). "Light variations of massive stars (alpha Cyg variables). XV. The LMC supergiants R99 (LBV), R103, R123 (LBV) and R128". Astronomy and Astrophysics. 332: 857–866. Bibcode:1998A&A...332..857V. ISSN   0004-6361.
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