HD 197911

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HD 197911
Cepheus constellation map.svg
Red circle.svg
Location of HD 197911 (circled)
Observation data
Epoch J2000 [1]        Equinox J2000 [1]
Constellation Cepheus
Right ascension 20h 43m 21.60554s
Declination +63° 12′ 32.8418″
Apparent magnitude  (V)7.669 [2]
Characteristics
Spectral type B5 [2]
B−V color index −0.01 [1]
J−H color index −0.109 [1]
J−K color index −0.107 [1]
Astrometry
Radial velocity (Rv)−3.80±3.5 km/s
Proper motion (μ)RA: −13.478 [3]   mas/yr
Dec.: -3.025 [3]   mas/yr
Parallax (π)1.0802 ± 0.0214  mas [3]
Distance 3,020 ± 60  ly
(930 ± 20  pc)
Details [2]
Mass 6.320±0.316  M☉
Radius 9.218±0.461  R☉
Other designations
AG+63° 1129, BD+62° 1854, Gaia DR3  2196984971452315392, GC  28915, HD  197911, HIP  102274, SAO  19003, PPM  22349, TIC  343565408, TYC  4250-1529-1, GSC  04250-01529, 2MASS J20432160+6312329 [1]
Database references
SIMBAD HD 197911

HD 197911 (HIP 102274) is a bluish-white hued star in the deep northern constellation of Cepheus, close to the border with Draco and Cygnus. With an apparent magnitude of 7.669, it is too faint to be seen by the naked eye under most conditions, but readily visible using binoculars. [4] The star is located some 3,020 light-years (930 parsecs) distant according to Gaia EDR3 parallax measurements, but is moving closer to the Solar System at a heliocentric radial velocity of −3.8±3.5  km/s .

The star appears close to the reflection nebula and H II region [5] Sh2-130, alongside the A0-type star HD 197809 and G5-type star SAO 18999, [6] though the latter two stars are located much closer to Earth at 469 ly (144 pc) [7] and 198 ly (61 pc), [8] respectively. The cluster itself is situated at a distance of 600 pc (2,000 ly). [6]

Properties and origin

HD 197911 is a massive B-type star with the spectral type B5, a mass 6.3 times that of the Sun and 9.2 times the radius. It is a runaway star traversing space at a peculiar velocity of 56.69 km/s. The star is thought to have once been part of a binary system, from which it was ejected as its companion ended its life in a supernova. [9]

Initially, the star was thought to have originated in an OB association called the Cepheus OB2 association, which it left 2–3 million years ago, when the association was 3–4 million years old. This aligned with the age of the Cepheus bubble, an annular structure of infrared emission, providing compelling evidence for the binary-supernova scenario, that is, that it was blasted out of a binary system by a companion going supernova. [10]

However, with updated astrometric data, it is now considered more likely that it formed in either Alessi-Teutsch 5 or NGC 7160, two star clusters that are each 12.5 and 9.0 million years old. Both origins are consistent with the initially proposed scenario. [9]

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References

  1. 1 2 3 4 5 6 "HD 197911". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 5 November 2024.
  2. 1 2 3 Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019). "Stellar and substellar companions of nearby stars from Gaia DR2". Astronomy & Astrophysics. 623. EDP Sciences: A72. doi: 10.1051/0004-6361/201834371 . ISSN   0004-6361. Record for this source at VizieR.
  3. 1 2 3 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.
  4. ↑ Zarenski, Ed (2004). "Limiting Magnitude in Binoculars" (PDF). Cloudy Nights. Archived (PDF) from the original on 21 July 2011. Retrieved 6 May 2011.
  5. ↑ Sharpless, Stewart (1959). "A Catalogue of H II Regions". The Astrophysical Journal Supplement Series. 4. American Astronomical Society: 257. doi:10.1086/190049. ISSN   0067-0049.
  6. 1 2 "Sh 2-130". galaxymap.org. Retrieved 5 November 2024.
  7. ↑ 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.
  8. ↑ 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.
  9. 1 2 Bhat, A.; Irrgang, A.; Heber, U. (2022). "The origin of early-type runaway stars from open clusters". Astronomy & Astrophysics. 663. EDP Sciences: A39. doi: 10.1051/0004-6361/202142993 . ISSN   0004-6361.
  10. ↑ Hoogerwerf, R.; de Bruijne, J. H. J.; de Zeeuw, P. T. (2001). "On the origin of the O and B-type stars with high velocities". Astronomy & Astrophysics. 365 (2). EDP Sciences: 49–77. doi: 10.1051/0004-6361:20000014 . ISSN   0004-6361.
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