HD 153261

In this article, we will explore the impact of HD 153261 on different aspects of contemporary society. From its influence on the economy to its relevance in the field of health, HD 153261 has played a fundamental role in shaping our world today. Through a comprehensive analysis, we will examine how HD 153261 has shaped our perceptions, behaviors and decisions, as well as its future projection. With this comprehensive approach, we aim to shed light on the complexity and scope of HD 153261, giving voice to diverse perspectives and enriching the debate around this topic of global resonance.

HD 153261

A light curve for HD 153261 from Hipparcos data, adapted from Lefèvre et al. (2009)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Ara
Right ascension 17h 01m 47.3875s[2]
Declination –58° 57′ 29.681″[2]
Apparent magnitude (V) 6.137[3]
Characteristics
Spectral type B1 V:ne[4] or B2 IVne[5]
U−B color index –0.956[3]
B−V color index –0.078[3]
Astrometry
Radial velocity (Rv)–6[6] km/s
Proper motion (μ) RA: –2.91[2] mas/yr
Dec.: –9.01[2] mas/yr
Parallax (π)2.32±0.38 mas[2]
Distanceapprox. 1,400 ly
(approx. 430 pc)
Details
Mass10.1 ± 0.3[5] M☉
Radius4.5[7] R☉
Luminosity (bolometric)11,045[8] L☉
Temperature21,150[8] K
Age20.4 ± 0.4[5] Myr
Other designations
CD–58 6607, HD 153261, HIP 83323, HR 6304, SAO 244362, V828 Arae.[9]
Database references
SIMBADdata

HD 153261 is the Henry Draper Catalogue designation for a star in the southern constellation of Ara. It has an apparent visual magnitude of 6.137,[3] placing it near the threshold of naked eye visibility. According to the Bortle Dark-Sky Scale, it can be viewed from dark suburban or rural skies. Based upon an annual parallax shift of just 2.32 mas,[2] it is located at a distance of around 1,400 light-years (430 parsecs) from Earth.

In 1983, Christopher Stagg reported that he suspected that HD 153261 is a variable star, and his later observations confirmed that it is in fact variable.[10][11] HD 153261 was given its variable star designation, V828 Arae, in 1987.[12]

This star has been catalogued with a stellar classification of B1 V:ne[4] or B2 IVne,[5] indicating that it is either a main sequence or a subgiant star. The 'n' indicates a nebulous spectrum created by the Doppler shift-broadened absorption lines from a rapid rotation, while the 'e' means this is a Be star, with the spectrum showing emission lines from hot, circumstellar gas. HD 153261 displays some variability with an amplitude of 0.090 in magnitude, and is a suspected spectroscopic binary.[1]

HD 153261 is a large star with over ten[5] times the Sun's mass and around 4.5[7] the radius of the Sun. It shines with more than 11,000[8] times the brightness of the Sun, with this energy being radiated into space at an effective temperature of 21,150 K.[8] At this heat, it glows with the blue-white hue of a B-type star.[13]

References

  1. ^ a b Lefèvre, L.; et al. (November 2009), "A systematic study of variability among OB-stars based on HIPPARCOS photometry", Astronomy and Astrophysics, 507 (2): 11411201, Bibcode:2009A&A...507.1141L, doi:10.1051/0004-6361/200912304.
  2. ^ a b c d e f van Leeuwen, F. (November 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.
  3. ^ a b c d Kozok, J. R. (September 1985), "Photometric observations of emission B-stars in the southern Milky Way", Astronomy and Astrophysics Supplement Series, 61: 387–405, Bibcode:1985A&AS...61..387K.
  4. ^ a b Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1975mcts.book.....H.
  5. ^ a b c d e Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  6. ^ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
  7. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics, 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  8. ^ a b c d Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  9. ^ "HR 6304". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2010-08-03.{{cite web}}: CS1 maint: postscript (link)
  10. ^ Stagg, C. (1983). "The southern Be star photometric campaign - A first report". Workshop on Rapid Variability of Early-Type Stars, Hvar, Yugoslavia, Sept. 19-23, 1983 Hvar Observatory, Bulletin (ISSN 0351-2651). 7 (1): 143. Bibcode:1983HvaOB...7..143S. Retrieved 25 November 2024.
  11. ^ Stagg, Christopher (July 1987). "A photometric survey of the bright southern Be stars". Monthly Notices of the Royal Astronomical Society. 227: 213–240. Bibcode:1987MNRAS.227..213S. doi:10.1093/mnras/227.1.213. Retrieved 25 November 2024.
  12. ^ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987). "The 68th Name-List of Variable Stars". Information Bulletin on Variable Stars. 3058: 1. Bibcode:1987IBVS.3058....1K. Retrieved 25 November 2024.
  13. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-07-21.