| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cepheus |
| Right ascension | 23h 00m 10.13337s [1] |
| Declination | +60° 55′ 38.4168″ [1] |
| Apparent magnitude (V) | 11.01 [2] |
| Characteristics | |
| Spectral type | WN8h [3] |
| B−V color index | +1.17 [2] |
| Astrometry | |
| Proper motion (μ) |
RA: −2.595±0.040
[4]
mas/
yr Dec.: −1.691±0.042 [4] mas/ yr |
| Parallax (π) | 0.2749 ± 0.0125 mas [5] |
| Distance | 11,900 ± 500
ly (3,600 ± 200 pc) |
| Absolute magnitude (MV) | −7.00 [6] |
| Details | |
| Mass | 32 [6] M☉ |
| Radius | 20.81 [6] R☉ |
| Luminosity | 1,023,000 [6] L☉ |
| Temperature | 39,800 [6] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 156 is a young massive and luminous Wolf–Rayet star in the constellation of Cepheus. Although it shows a WR spectrum, it is thought to be a young star still fusing hydrogen in its core.
Distance
WR 156 has a Hipparcos parallax of 3.16" indicating a distance of about a thousand light years, although with a fairly large margin of error. Other studies indicate that it is much more distant based on a very high luminosity and faint apparent magnitude. [6] The Gaia DR1 parallax is 0.07". The margin of error is larger than the measured parallax, but still the indication is for a very large distance. [7] In Gaia Data Release 2, the parallax is given as 0.2090±0.0251 mas but with a marker that the result may be unreliable. [4] In the Gaia Early Release 3, the solution was adjusted to 0.2749±0.0125 mas, still with significant astrometric noise excess. [5]
Physical properties
WR 156 has a WR spectrum on the nitrogen sequence, indicating strong emission of helium and nitrogen, but it also shows features of hydrogen. Therefore, it is given a spectral type of WN8h. Its outer layers are calculated to contain 30% hydrogen, one of the highest levels for any galactic Wolf Rayet star. [8]
WR 156 has a low temperature and slow stellar wind by Wolf Rayet standards, only 39,800 K and 660 km/s respectively. The wind is very dense, with total mass loss of more than 1/100,000 M☉/year. [6]
WR 156 is a young hydrogen-rich star, still burning hydrogen in its core but sufficiently luminous to have convected up nitrogen and helium fusion products to its surface. It shows 27% hydrogen at its surface. [6] It is estimated to have had an initial mass of 50 M☉ several million years ago. [8]
References
- ^ a b 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.
- ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode: 2000A&A...355L..27H. doi: 10.1888/0333750888/2862. ISBN 0333750888.
- ^ Maryeva, Olga (2016). "The study of massive stars with 50 Msun initial mass at different evolutionary stages". arXiv: 1612.01191 [ astro-ph.SR].
- ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b 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. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d e f g h Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv: 1904.04687. Bibcode: 2019A&A...625A..57H. doi: 10.1051/0004-6361/201834850. S2CID 104292503.
- ^ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally Published in: Astron. Astrophys. 1337. Bibcode: 2016yCat.1337....0G.
- ^ a b Maryeva, O. V.; Afanasiev, V. L.; Panchuk, V. E. (2013). "Study of the late nitrogen-sequence Galactic Wolf-Rayet star WR156. Spectropolarimetry and modeling". New Astronomy. 25: 27–31. Bibcode: 2013NewA...25...27M. doi: 10.1016/j.newast.2013.03.015.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cepheus |
| Right ascension | 23h 00m 10.13337s [1] |
| Declination | +60° 55′ 38.4168″ [1] |
| Apparent magnitude (V) | 11.01 [2] |
| Characteristics | |
| Spectral type | WN8h [3] |
| B−V color index | +1.17 [2] |
| Astrometry | |
| Proper motion (μ) |
RA: −2.595±0.040
[4]
mas/
yr Dec.: −1.691±0.042 [4] mas/ yr |
| Parallax (π) | 0.2749 ± 0.0125 mas [5] |
| Distance | 11,900 ± 500
ly (3,600 ± 200 pc) |
| Absolute magnitude (MV) | −7.00 [6] |
| Details | |
| Mass | 32 [6] M☉ |
| Radius | 20.81 [6] R☉ |
| Luminosity | 1,023,000 [6] L☉ |
| Temperature | 39,800 [6] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WR 156 is a young massive and luminous Wolf–Rayet star in the constellation of Cepheus. Although it shows a WR spectrum, it is thought to be a young star still fusing hydrogen in its core.
Distance
WR 156 has a Hipparcos parallax of 3.16" indicating a distance of about a thousand light years, although with a fairly large margin of error. Other studies indicate that it is much more distant based on a very high luminosity and faint apparent magnitude. [6] The Gaia DR1 parallax is 0.07". The margin of error is larger than the measured parallax, but still the indication is for a very large distance. [7] In Gaia Data Release 2, the parallax is given as 0.2090±0.0251 mas but with a marker that the result may be unreliable. [4] In the Gaia Early Release 3, the solution was adjusted to 0.2749±0.0125 mas, still with significant astrometric noise excess. [5]
Physical properties
WR 156 has a WR spectrum on the nitrogen sequence, indicating strong emission of helium and nitrogen, but it also shows features of hydrogen. Therefore, it is given a spectral type of WN8h. Its outer layers are calculated to contain 30% hydrogen, one of the highest levels for any galactic Wolf Rayet star. [8]
WR 156 has a low temperature and slow stellar wind by Wolf Rayet standards, only 39,800 K and 660 km/s respectively. The wind is very dense, with total mass loss of more than 1/100,000 M☉/year. [6]
WR 156 is a young hydrogen-rich star, still burning hydrogen in its core but sufficiently luminous to have convected up nitrogen and helium fusion products to its surface. It shows 27% hydrogen at its surface. [6] It is estimated to have had an initial mass of 50 M☉ several million years ago. [8]
References
- ^ a b 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.
- ^ a b Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode: 2000A&A...355L..27H. doi: 10.1888/0333750888/2862. ISBN 0333750888.
- ^ Maryeva, Olga (2016). "The study of massive stars with 50 Msun initial mass at different evolutionary stages". arXiv: 1612.01191 [ astro-ph.SR].
- ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b 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. (Erratum: doi: 10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d e f g h Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv: 1904.04687. Bibcode: 2019A&A...625A..57H. doi: 10.1051/0004-6361/201834850. S2CID 104292503.
- ^ Gaia Collaboration (2016). "VizieR Online Data Catalog: Gaia DR1 (Gaia Collaboration, 2016)". VizieR On-line Data Catalog: I/337. Originally Published in: Astron. Astrophys. 1337. Bibcode: 2016yCat.1337....0G.
- ^ a b Maryeva, O. V.; Afanasiev, V. L.; Panchuk, V. E. (2013). "Study of the late nitrogen-sequence Galactic Wolf-Rayet star WR156. Spectropolarimetry and modeling". New Astronomy. 25: 27–31. Bibcode: 2013NewA...25...27M. doi: 10.1016/j.newast.2013.03.015.