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HD 89890

A visual band light curve for MV Velorum, adapted from Sterken et al. (1996) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Vela
Right ascension 10h 20m 54.77319s [2]
Declination −56° 02′ 35.5728″ [2]
Apparent magnitude (V) 4.50 [3]
Characteristics
Spectral type B3 III + A0 IVpSi + A2 + K0 III [4]
B−V color index −0.102±0.014 (A + B) [5]
Astrometry
Radial velocity (Rv)+10.4±2.8 [5] km/s
Proper motion (μ) RA: −7.5 [6]  mas/ yr
Dec.: +4.0 [6]  mas/ yr
Parallax (π)2.6564 ± 0.2314  mas [2]
Distance1,200 ± 100  ly
(380 ± 30  pc)
Absolute magnitude (MV)−3.21 (A + B) [5]
Details
A (HD 89890)
Radius10.07±0.20 [7]  R☉
Luminosity3,082.41 [5]  L☉
Surface gravity (log g)3.00±0.03 [7]  cgs
Temperature15,000±150 [7]  K
Rotational velocity (v sin i)26.8±0.5 [7] km/s
Other designations
WDS J10209-5603 [8]
A+B: CPD−55 3286, HIP 50676, HR 4074 [8]
A: J Velorum, MV Velorum, HD 89890, SAO 237959, TYC 8604-975-1 [8]
B: SAO 237960, TYC 8604-2444-1 [8]
C: CD−55 3306, SAO 237958, TYC 8604-2137-1 [8]
Database references
SIMBAD HD 89890 (A)
HIC 50676 (A+B)
TYC 8604-2444-1 (B)
CD-55 3306 (C)

HD 89890 is the brightest member of a multiple star system with at least four components, [4] located in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.50. [3] The annual parallax shift of 2.6  mas [2] provides a distance estimate of around 1,200 light-years (370 parsecs). It is moving further away from Earth with a heliocentric radial velocity of +10 km/s. [5]

System

The Washington Double Star Catalog lists three visible components for this system. The brightest, component A, is of visual magnitude 4.50. Component B has a magnitude of 7.179, [9] and as of 2000 lies at an angular separation of 7.10 ″ from A, along a position angle (PA) of 102°. Component C is a magnitude 9.125 star [9] at a separation of 36.20″ from A at a PA of 191°. The physical link between the stars was described on the basis of their dynamic parallax and mean velocities. [10] The three components A, B and C have Gaia Data Release 2 parallaxes of 2.6564±0.2314  mas, 2.1771±0.0490 mas, and 1.6097±0.0400 mas, respectively. [2]

Properties

Component A has a stellar classification of B3 III, and is categorized as a Be star. It shows photometric variations with multiple periods around 4.6 days and line-profile variations with a period of 2.318 days. The radial velocity of this star is constant. [4] It has 10 [7] times the Sun's radius and shines with 3,082 [5] times the Sun's luminosity from its photosphere at an effective temperature of 15,000  K. [7]

The component B shows a variation in spectra consistent with being a double-lined spectroscopic binary. The brighter member (Ba) is a silicon star with a class of A0 IVpSi, while the fainter component (Bb) is of type A2. Component C has a class of K0 III, indicating it is an evolved giant star. The measured effective temperature of C is 5,500 K. The fact that component A most likely shares a common origin with C suggests that the former is much older than expected, and may actually be a blue straggler formed from the merger of a close binary. This could have been caused by the gravitational influence of an unseen companion of A. [4]

References

  1. ^ Sterken, C.; Vogt, N.; Mennickent, R. E. (July 1996). "Long-term photometry of Be stars. II. Periodic variations on time scales of days to months". Astronomy and Astrophysics. 311: 579–586. Bibcode: 1996A&A...311..579S. Retrieved 30 April 2022.
  2. ^ a b c d e 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.
  3. ^ a b Jaschek, M; Egret, D; Jaschek, M; Groth, H. -G (1982). "Catalog of Be stars". Be Stars. 98: 261–263. Bibcode: 1982IAUS...98..261J. doi: 10.1007/978-94-009-8565-0_44 (inactive 2024-06-09). ISBN  978-90-277-1367-4.{{ cite journal}}: CS1 maint: DOI inactive as of June 2024 ( link)
  4. ^ a b c d Veramendi, M. E.; González, J. F. (July 2014), "Spectroscopic study of early-type multiple stellar systems. II. New binary subsystems", Astronomy & Astrophysics, 567: 10, arXiv: 1405.1084, Bibcode: 2014A&A...567A..35V, doi: 10.1051/0004-6361/201423736, S2CID  21711755, A35.
  5. ^ a b c d e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971, Bibcode: 2012AstL...38..331A, doi: 10.1134/S1063773712050015, S2CID  119257644.
  6. ^ a b Röser, S.; Bastian, U. (September 1988), "A New Star Catalogue of SAO Type", Astronomy and Astrophysics Supplement Series, 74: 449, Bibcode: 1988A&AS...74..449R.
  7. ^ a b c d e f Arcos, C.; et al. (March 2018), "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society, 474 (4): 5287–5299, arXiv: 1711.08675, Bibcode: 2018MNRAS.474.5287A, doi: 10.1093/mnras/stx3075, S2CID  74872624.
  8. ^ a b c d e "HD 89890". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-08.
  9. ^ a b Høg, E.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode: 2000A&A...355L..27H. doi: 10.1888/0333750888/2862. ISBN  978-0333750889.
  10. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
Retrieved from " https://en.wikipedia.org/?title=HD_89890&oldid=1228137934"
From Wikipedia, the free encyclopedia
(Redirected from MV Velorum)
HD 89890

A visual band light curve for MV Velorum, adapted from Sterken et al. (1996) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Vela
Right ascension 10h 20m 54.77319s [2]
Declination −56° 02′ 35.5728″ [2]
Apparent magnitude (V) 4.50 [3]
Characteristics
Spectral type B3 III + A0 IVpSi + A2 + K0 III [4]
B−V color index −0.102±0.014 (A + B) [5]
Astrometry
Radial velocity (Rv)+10.4±2.8 [5] km/s
Proper motion (μ) RA: −7.5 [6]  mas/ yr
Dec.: +4.0 [6]  mas/ yr
Parallax (π)2.6564 ± 0.2314  mas [2]
Distance1,200 ± 100  ly
(380 ± 30  pc)
Absolute magnitude (MV)−3.21 (A + B) [5]
Details
A (HD 89890)
Radius10.07±0.20 [7]  R☉
Luminosity3,082.41 [5]  L☉
Surface gravity (log g)3.00±0.03 [7]  cgs
Temperature15,000±150 [7]  K
Rotational velocity (v sin i)26.8±0.5 [7] km/s
Other designations
WDS J10209-5603 [8]
A+B: CPD−55 3286, HIP 50676, HR 4074 [8]
A: J Velorum, MV Velorum, HD 89890, SAO 237959, TYC 8604-975-1 [8]
B: SAO 237960, TYC 8604-2444-1 [8]
C: CD−55 3306, SAO 237958, TYC 8604-2137-1 [8]
Database references
SIMBAD HD 89890 (A)
HIC 50676 (A+B)
TYC 8604-2444-1 (B)
CD-55 3306 (C)

HD 89890 is the brightest member of a multiple star system with at least four components, [4] located in the southern constellation of Vela. It is visible to the naked eye with an apparent visual magnitude of 4.50. [3] The annual parallax shift of 2.6  mas [2] provides a distance estimate of around 1,200 light-years (370 parsecs). It is moving further away from Earth with a heliocentric radial velocity of +10 km/s. [5]

System

The Washington Double Star Catalog lists three visible components for this system. The brightest, component A, is of visual magnitude 4.50. Component B has a magnitude of 7.179, [9] and as of 2000 lies at an angular separation of 7.10 ″ from A, along a position angle (PA) of 102°. Component C is a magnitude 9.125 star [9] at a separation of 36.20″ from A at a PA of 191°. The physical link between the stars was described on the basis of their dynamic parallax and mean velocities. [10] The three components A, B and C have Gaia Data Release 2 parallaxes of 2.6564±0.2314  mas, 2.1771±0.0490 mas, and 1.6097±0.0400 mas, respectively. [2]

Properties

Component A has a stellar classification of B3 III, and is categorized as a Be star. It shows photometric variations with multiple periods around 4.6 days and line-profile variations with a period of 2.318 days. The radial velocity of this star is constant. [4] It has 10 [7] times the Sun's radius and shines with 3,082 [5] times the Sun's luminosity from its photosphere at an effective temperature of 15,000  K. [7]

The component B shows a variation in spectra consistent with being a double-lined spectroscopic binary. The brighter member (Ba) is a silicon star with a class of A0 IVpSi, while the fainter component (Bb) is of type A2. Component C has a class of K0 III, indicating it is an evolved giant star. The measured effective temperature of C is 5,500 K. The fact that component A most likely shares a common origin with C suggests that the former is much older than expected, and may actually be a blue straggler formed from the merger of a close binary. This could have been caused by the gravitational influence of an unseen companion of A. [4]

References

  1. ^ Sterken, C.; Vogt, N.; Mennickent, R. E. (July 1996). "Long-term photometry of Be stars. II. Periodic variations on time scales of days to months". Astronomy and Astrophysics. 311: 579–586. Bibcode: 1996A&A...311..579S. Retrieved 30 April 2022.
  2. ^ a b c d e 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.
  3. ^ a b Jaschek, M; Egret, D; Jaschek, M; Groth, H. -G (1982). "Catalog of Be stars". Be Stars. 98: 261–263. Bibcode: 1982IAUS...98..261J. doi: 10.1007/978-94-009-8565-0_44 (inactive 2024-06-09). ISBN  978-90-277-1367-4.{{ cite journal}}: CS1 maint: DOI inactive as of June 2024 ( link)
  4. ^ a b c d Veramendi, M. E.; González, J. F. (July 2014), "Spectroscopic study of early-type multiple stellar systems. II. New binary subsystems", Astronomy & Astrophysics, 567: 10, arXiv: 1405.1084, Bibcode: 2014A&A...567A..35V, doi: 10.1051/0004-6361/201423736, S2CID  21711755, A35.
  5. ^ a b c d e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971, Bibcode: 2012AstL...38..331A, doi: 10.1134/S1063773712050015, S2CID  119257644.
  6. ^ a b Röser, S.; Bastian, U. (September 1988), "A New Star Catalogue of SAO Type", Astronomy and Astrophysics Supplement Series, 74: 449, Bibcode: 1988A&AS...74..449R.
  7. ^ a b c d e f Arcos, C.; et al. (March 2018), "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society, 474 (4): 5287–5299, arXiv: 1711.08675, Bibcode: 2018MNRAS.474.5287A, doi: 10.1093/mnras/stx3075, S2CID  74872624.
  8. ^ a b c d e "HD 89890". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-08-08.
  9. ^ a b Høg, E.; et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode: 2000A&A...355L..27H. doi: 10.1888/0333750888/2862. ISBN  978-0333750889.
  10. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920.
Retrieved from " https://en.wikipedia.org/?title=HD_89890&oldid=1228137934"

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