AS 314

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V452 Scuti
Observation data
Epoch J2000      Equinox J2000
Constellation Scutum
Right ascension 18h 39m 26.10612s[1]
Declination −13° 50′ 47.1892″[1]
Apparent magnitude (V) 9.85[2]
Characteristics
Spectral type Protoplanetary nebula[3]
U−B color index +0.12[2]
B−V color index +0.89[2]
Variable type cLBV[4]
Astrometry
Radial velocity (Rv)−77±8[5] km/s
Proper motion (μ) RA: -4.416[5] mas/yr
Dec.: -6.241[5] mas/yr
Parallax (π)0.5853 ± 0.0141[5] mas
Distance5,600 ± 100 ly
(1,710 ± 40 pc)
Details
Luminosity3200[3] L☉
Temperature10,200[6] K
Other designations
V452 Sct, BD -13°5061, HIP 91477, 2MASS J18392610-1350470
Database references
SIMBADdata

AS 314, also known as V452 Scuti, is a protoplanetary nebula[3] 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.

Characteristics[]

AS 314 was poorly studied until the year 2000, when Miroshnichenko et al. incorrectly estimated a distance for this star of around 10 kiloparsecs (32,600 light years), a luminosity 160,000 times that of Sun (L☉), a radius 200 times the solar radius (R☉), and an initial mass of 20 solar masses (M☉). It was also estimated to be losing 2 × 10−5 M☉ each year (in other words, 1 M☉ every 50,000 years) through a very strong stellar wind.[7]

AS 314 has an infrared excess, suggesting that it's shrouded in a circumstellar envelope of dust.[7][8] however, it has not been classified as a bona fide luminous blue variable, but as a candidate.[4]

The Hipparcos parallax and proper motions are large and imply a much closer, and hence less luminous, star.[1] The Hipparcos measurement was later confirmed by the Gaia mission,[5] reclassifying AS 314 as post-AGB star.[3]

References[]

  1. ^ a b c Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c Kozok, J. R. (1985). "Photometric observations of emission B-stars in the southern Milky Way". Astronomy and Astrophysics Supplement Series. 61: 387. Bibcode:1985A&AS...61..387K.
  3. ^ a b c d Groh, Jose H.; Stassun, Keivan G.; Drout, Maria R.; Murphy, Jeremiah W.; Aghakhanloo, Mojgan; Smith, Nathan (2019), "On the Gaia DR2 distances for Galactic luminous blue variables", Monthly Notices of the Royal Astronomical Society, 488 (2): 1760–1778, arXiv:1805.03298, doi:10.1093/mnras/stz1712
  4. ^ a b Nazé, Y.; Rauw, G.; Hutsemékers, D. (2012). "The first X-ray survey of Galactic luminous blue variables". Astronomy & Astrophysics. 538: A47. arXiv:1111.6375. Bibcode:2012A&A...538A..47N. doi:10.1051/0004-6361/201118040. S2CID 43688343.
  5. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. Gaia EDR3 record for this source at VizieR.
  6. ^ van Genderen, A.M. (2001). "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.
  7. ^ a b Miroshnichenko, A. S.; Chentsov, E. L.; Klochkova, V. G. (2000). "AS?314: A dusty A?type hypergiant" (PDF). Astronomy and Astrophysics Supplement Series. 144 (3): 379. Bibcode:2000A&AS..144..379M. doi:10.1051/aas:2000216.
  8. ^ Clark, J. S.; Larionov, V. M.; Arkharov, A. (May 2005). "On the population of galactic Luminous Blue Variables" (PDF). Astronomy and Astrophysics. 435 (1): 239–246. Bibcode:2005A&A...435..239C. doi:10.1051/0004-6361:20042563.
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