HD 92206

Last updated

HD 92206
Carina constellation map.svg
Red circle.svg
Location of HD 92206 (circled)
Observation data
Epoch J2000 [1]        Equinox J2000 [1]
Constellation Carina
HD 92206A
Right ascension 10h 37m 22.28065s
Declination −58° 37′ 22.8526″
Apparent magnitude  (V)+8.219 [2]
HD 92206B
Right ascension 10h 37m 22.96508s [3]
Declination −58° 37′ 22.9596″ [3]
HD 92206C
Right ascension 06h 13m 47.17685s [4]
Declination −58° 37′ 22.9596″ [4]
Apparent magnitude  (V)8.966 [2]
Characteristics
HD 92206A
Spectral type O6.5V + O6.5V, [5] O6V((f))z (combined) [6]
B−V color index 0.096 [2]
J−H color index −0.025 [7]
J−K color index 0.084 [7]
HD 92206B
Spectral type O6.5V [8] or O6V((f))z [6]
J−H color index 0.163 [7]
J−K color index −0.047 [7]
HD 92206C
Spectral type O8V + O9.7V + B2: [9]
B−V color index 0.119 [2]
J−H color index 0.064 [7]
J−K color index 0.084 [7]
Astrometry
HD 92206A
Proper motion (μ)RA: -7.290 [1]   mas/yr
Dec.: 2.814 [1]   mas/yr
Parallax (π)0.3881 ± 0.0217  mas [1]
Distance 8,400 ± 500  ly
(2,600 ± 100  pc)
HD 92206B
Proper motion (μ)RA: -7.176 [3]   mas/yr
Dec.: 2.844 [3]   mas/yr
Parallax (π)0.4395 ± 0.015  mas [3]
Distance 7,400 ± 300  ly
(2,280 ± 80  pc)
HD 92206C
Proper motion (μ)RA: -7.538 [4]   mas/yr
Dec.: 2.206 [4]   mas/yr
Parallax (π)0.6476 ± 0.0866  mas [4]
Distance approx. 5,000  ly
(approx. 1,500  pc)
Orbit [9]
PrimaryHD 92206C O8V
CompanionHD 92206C O9.7V
Period (P)2.022504(12)  d
Semi-major axis (a)21.8±0.4 R☉
Eccentricity (e)0
Semi-amplitude (K1)
(primary)		209.3±4.6 km/s
Semi-amplitude (K2)
(secondary)		289.1±7.8 km/s
Details
HD 92206A
Luminosity 170,000 (bolometric) [8]   L☉
Age ≲1 [10]   Myr
HD 92206A2
Mass 0.5-1 [8]   M☉
Age ~1 [8]   Myr
HD 92206B
Luminosity 170,000 (bolometric) [8]   L☉
HD 92206C O8V
Luminosity112,000 (bolometric) [8]   L☉
Rotational velocity (v sin i)146±30 [9]  km/s
HD 92206C O9.7V
Rotational velocity (v sin i)120±5 [9]  km/s
HD 92206C B2
Rotational velocity (v sin i)67±8 [9]  km/s
Other designations
CD−57° 3380, CPD−57° 3584, GC  14621, HD  92206, SAO  238269, PPM  339253, WDS J10374-5837AB, GSC  08613-01825, NGC 3324 2, ALS 1697 [11]
HD 92206A: CD−57° 3380A, Gaia DR3  5350671494307479808, HD  92206A, CCDM J10374-5837A, WDS J10374-5837A, TIC  458230570, TYC  8613-1825-1, 2MASS J10372226-5837229 [12]
HD 92206B: CD−57° 3380B, CPD−57° 3584B, Gaia DR3  5350671498620168448, HD  92206B, WDS J10374-5837B, TIC  458230572, 2MASS J10372295-5837230, NGC 3324 5, ALS 17532 [13]
HD 92206C: CD−57° 3378, CPD−57° 3580, Gaia DR3  5350671459947742336, GC  14618, HD  92206C, SAO  238266, PPM  339247, TIC  458230632, TYC  8613-780-1, GSC  08613-00780, 2MASS J10371860-5837419, NGC 3324 4, LS 1695 [14] [9]
Database references
SIMBAD A
B
C

HD 92206 is a Henry Draper Catalogue designation given to a collection of stars in the southern constellation of Carina. It consists of two systems; HD 92206AB, where component A is itself a spectroscopic binary; [5] and the trinary HD 92206C. [9] They are the brightest stars in NGC 3324 and the ionizing stars of the associated emission nebula Gum 31 (IC 2599). [5] The relationship between AB and C is disputed: some state that they are all part of a singular multiple star system, [15] whereas others treat AB and C as neighboring star systems that together "form a compact group." [16] All of their components are young (age ≲1 Myr [10] ), massive OB stars near the zero-age main sequence. [5] Two other objects, HD 92206A2 and C2, have been discovered in the immediate vicinity, which are both likely less massive late-type stars based on their X-ray profile. [8]

Contents

Stellar components

HD 92206AB

HD 92206A and B comprise a wide binary system, separated by 5".4. [16] They have both been given the spectral type of O6.5V, indicating they are both energetic O-type main-sequence stars each radiating a bolometric luminosity about 170,000 times the Sun's. [8] Despite this, A appears almost a magnitude brighter than B, thus it has been suggested that A could be a spectroscopic binary between two similar O6.5V stars. [5]

In 2014, an X-ray source, designated HD 92206A2, was identified just 0".83 (distance ~1900 AU) from A, which emits hard X-rays i.e., X-rays with a high photon energy at 5.17 keV (wavelength 0.240 nm), as opposed to the soft (low-energy) X-rays released by late O-type stars like A, B, and C. Unless it is highly reddened, this is thought to be a young (~1 Myr old) star with a mass of 0.5–1 M☉, producing X-rays in its corona. [8]

HD 92206C

At a separation of 33" from the AB pair, HD 92206C (alternatively CPD−57° 3580 [9] ) was first reported to be a spectroscopic binary in 2007, [16] and was further resolved to be a triple system by 2017. Two stars with the spectral types O8V and O9.7V orbit each other with a period of 2.02 days, while a fainter B2-type star orbits them within 1 arcsecond of the inner pair. [9] The brightest of the three has a luminosity 112,000 times that of the Sun (though this was derived from a spectral type of O7.5V rather than O8V). [8] The spectrum of C shows very strong, broad hydrogen lines resembling that of θ1 Orionis C, characteristic of very young stars. The star (or at least one of its components), alongside the white supergiant HD 92207, is known to have a magnetic field. [15]

Simultaneously with the detection of HD 92206A2, another X-ray source, C2, was discovered 1".7 from C, but its closeness to the much brighter C prevented precise measurements. Due to its faintness, it is thought to be a late-type star. [8]

Formation

The location of the HD 92206 system is offset from the center of Gum 31, the nebula from which it formed. To explain this, it has been theorized that the stars were born as two molecular clouds with differing velocities collided at supersonic speeds about one million years ago, which carved a cavity into the center of the nebula and shaped a core that collapsed to form the massive stars. [10]

Bow shock

In 2005, a bow shock was discovered to surround the multiple system. It has a thickness of 98000±27000  km , extremely thin compared to the bow shocks around other stars reported in the same paper, which are tens or hundreds of AU thick. Due to its great distance from Earth, it has not been fully resolved. [17]

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References

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  2. 1 2 3 4 Høg, E.; et al. (February 2000). "The Tycho-2 Catalogue of the 2.5 Million Brightest Stars". Astronomy and Astrophysics. 355 (1): L27 –L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 3 4 5 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. 1 2 3 4 5 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.
  5. 1 2 3 4 5 Cappa, C.; Niemela, V. S.; Amorín, R.; Vasquez, J. (2008). "The environs of the H II region Gum 31" (PDF). Astronomy & Astrophysics. 477 (1): 173–183. doi: 10.1051/0004-6361:20067028 . ISSN   0004-6361 . Retrieved 27 December 2024.
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  8. 1 2 3 4 5 6 7 8 9 10 11 Preibisch, T.; Mehlhorn, M.; Townsley, L.; Broos, P.; Ratzka, T. (2014). "Chandra X-ray observation of the H ii region Gum 31 in the Carina nebula complex" (PDF). Astronomy & Astrophysics. 564: A120. doi: 10.1051/0004-6361/201323133 . ISSN   0004-6361 . Retrieved 27 December 2024.
  9. 1 2 3 4 5 6 7 8 9 Mayer, Pavel; Harmanec, Petr; Chini, Rolf; Nasseri, Anita; Nemravová, Jana A.; Drechsel, Horst; Catalan-Hurtado, Rodrigo; Barlow, Brad N.; Frémat, Yves; Kotková, Lenka (2017). "Physical properties of seven binary and higher-order multiple OB systems" (PDF). Astronomy & Astrophysics. 600: A33. doi: 10.1051/0004-6361/201628852 . ISSN   0004-6361 . Retrieved 27 December 2024.
  10. 1 2 3 Fujita, Shinji; Sano, Hidetoshi; Enokiya, Rei; Hayashi, Katsuhiro; Kohno, Mikito; Tsuge, Kisetsu; Tachihara, Kengo; Nishimura, Atsushi; Ohama, Akio; Yamane, Yumiko; Ohno, Takahiro; Yamada, Rin I; Fukui, Yasuo (4 October 2021). "Massive star formation in the Carina nebula complex and Gum 31. II. A cloud–cloud collision in Gum 31". Publications of the Astronomical Society of Japan. 73 (5): 1255–1261. doi: 10.1093/pasj/psab071 . ISSN   0004-6264 . Retrieved 27 December 2024.
  11. ↑ "HD 92206". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 December 2024.
  12. ↑ "HD 92206A". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 December 2024.
  13. ↑ "HD 92206B". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 December 2024.
  14. ↑ "CD-57+3378". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 31 December 2024.
  15. 1 2 Hubrig, S.; Schöller, M.; Ilyin, I.; Kharchenko, N. V.; Oskinova, L. M.; Langer, N.; González, J. F.; Kholtygin, A. F.; Briquet, M.; collaboration, the MAGORI (2013). "Exploring the origin of magnetic fields in massive stars: II. New magnetic field measurements in cluster and field stars⋆" (PDF). Astronomy & Astrophysics. 551: A33. doi: 10.1051/0004-6361/201220721 . ISSN   0004-6361 . Retrieved 27 December 2024.
  16. 1 2 3 Campillay, A.; Arias, J. I.; Barbá, Rodolfo; Gamen, R. C.; Morrell, N.; Maíz Apellániz, Jesús; Walborn, N.; Sota, Alfredo; Alfaro, Emilio J. (January 2007). HD 92206C: a new short-period massive binary in the Carina Nebula. VI Reunion Anual Sociedad Chilena de Astronomia (SOCHIAS). Bibcode:2007soch.conf...63C.
  17. ↑ Brown, D.; Bomans, D. J. (2005). "To see or not to see a bow shock: Identifying bow shocks with H α allsky surveys" (PDF). Astronomy & Astrophysics. 439 (1): 183–194. doi: 10.1051/0004-6361:20041054 . ISSN   0004-6361 . Retrieved 27 December 2024.
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