From Wikipedia, the free encyclopedia
Omicron Lupi
Observation data
Epoch J2000.0       Equinox J2000.0 ( ICRS)
Constellation Lupus
Right ascension 14h 51m 38.30289s [1]
Declination −43° 34′ 31.2965″ [1]
Apparent magnitude (V) 4.323 [2] (4.84 + 5.27) [3]
Characteristics
Spectral type B5 IV [3]
U−B color index −0.620 [2]
B−V color index −0.159 [2]
Astrometry
Radial velocity (Rv)+7.30±0.74 [4] km/s
Proper motion (μ) RA: −25.20 [1]  mas/ yr
Dec.: −27.13 [1]  mas/ yr
Parallax (π)8.07 ± 0.59  mas [1]
Distance400 ± 30  ly
(124 ± 9  pc)
Absolute magnitude (MV)−1.2±0.3 [5]
Details
Mass5.7±0.2 [5]  M
Radius3.5 [5]  R
Luminosity1,260 [5]  L
Surface gravity (log g)4.1±0.1 [5]  cgs
Temperature18,000 [6]  K
Rotational velocity (v sin i)25 [6] km/s
Other designations
ο Lup, CD−43° 9391, HD 130807, HIP 72683, HR 5528, SAO 225248. [7]
Database references
SIMBAD data

Omicron Lupi (ο Lup) is a binary star [3] in the southern constellation of Lupus. It is a visible to the naked eye with a combined apparent visual magnitude of 4.323. [2] Based upon an annual parallax shift of 8.07  mas as seen from Earth, [1] it is located around 400  light-years from the Sun, give or take 30 light-years. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.13±0.01 due to interstellar dust. [5] It is a member of the Upper Centaurus–Lupus [8] subgroup of the nearby Scorpius–Centaurus association. [6]

This is a visual binary star system with the components having an angular separation of 0.1  arcsecond. [8] The primary, component A, is a magnitude 4.84 B-type subgiant star with a stellar classification of B5 V. [3] It displays radial velocity variations indicating it has an unseen second companion orbiting at a separation of at least 17  AU with a period of 27 years or more. [6] The spectrum of the primary displays a Zeeman effect indicating a magnetic field with a strength ranging from −94 to 677 G. [6] The visible companion, component B, has a visual magnitude of 5.27. [3]

References

  1. ^ a b c d e f 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.
  2. ^ a b c d Cousins, A. W. J. (1973), "Revised zero points and UBV photometry of stars in the Harvard E and F regions", Memoirs of the Royal Astronomical Society, 77: 223–236, Bibcode: 1973MmRAS..77..223C.
  3. ^ a b c d e Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
  4. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048, Bibcode: 2012A&A...546A..61D, doi: 10.1051/0004-6361/201219219, S2CID  59451347, A61.
  5. ^ a b c d e f Petit, V.; et al. (February 2013), "A magnetic confinement versus rotation classification of massive-star magnetospheres" (PDF), Monthly Notices of the Royal Astronomical Society, 429 (1): 398–422, arXiv: 1211.0282, Bibcode: 2013MNRAS.429..398P, doi: 10.1093/mnras/sts344.
  6. ^ a b c d e Alecian, E.; et al. (December 2011), "First HARPSpol discoveries of magnetic fields in massive stars", Astronomy & Astrophysics, 536: 4, arXiv: 1111.3433, Bibcode: 2011A&A...536L...6A, doi: 10.1051/0004-6361/201118354, S2CID  51173988, L6.
  7. ^ "omi Lup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-10.
  8. ^ a b Chen, Christine H.; et al. (September 2012), "A Spitzer MIPS Study of 2.5-2.0 M Stars in Scorpius–Centaurus", The Astrophysical Journal, 756 (2): 24, arXiv: 1207.3415, Bibcode: 2012ApJ...756..133C, doi: 10.1088/0004-637X/756/2/133, S2CID  119278056, 133.
From Wikipedia, the free encyclopedia
Omicron Lupi
Observation data
Epoch J2000.0       Equinox J2000.0 ( ICRS)
Constellation Lupus
Right ascension 14h 51m 38.30289s [1]
Declination −43° 34′ 31.2965″ [1]
Apparent magnitude (V) 4.323 [2] (4.84 + 5.27) [3]
Characteristics
Spectral type B5 IV [3]
U−B color index −0.620 [2]
B−V color index −0.159 [2]
Astrometry
Radial velocity (Rv)+7.30±0.74 [4] km/s
Proper motion (μ) RA: −25.20 [1]  mas/ yr
Dec.: −27.13 [1]  mas/ yr
Parallax (π)8.07 ± 0.59  mas [1]
Distance400 ± 30  ly
(124 ± 9  pc)
Absolute magnitude (MV)−1.2±0.3 [5]
Details
Mass5.7±0.2 [5]  M
Radius3.5 [5]  R
Luminosity1,260 [5]  L
Surface gravity (log g)4.1±0.1 [5]  cgs
Temperature18,000 [6]  K
Rotational velocity (v sin i)25 [6] km/s
Other designations
ο Lup, CD−43° 9391, HD 130807, HIP 72683, HR 5528, SAO 225248. [7]
Database references
SIMBAD data

Omicron Lupi (ο Lup) is a binary star [3] in the southern constellation of Lupus. It is a visible to the naked eye with a combined apparent visual magnitude of 4.323. [2] Based upon an annual parallax shift of 8.07  mas as seen from Earth, [1] it is located around 400  light-years from the Sun, give or take 30 light-years. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.13±0.01 due to interstellar dust. [5] It is a member of the Upper Centaurus–Lupus [8] subgroup of the nearby Scorpius–Centaurus association. [6]

This is a visual binary star system with the components having an angular separation of 0.1  arcsecond. [8] The primary, component A, is a magnitude 4.84 B-type subgiant star with a stellar classification of B5 V. [3] It displays radial velocity variations indicating it has an unseen second companion orbiting at a separation of at least 17  AU with a period of 27 years or more. [6] The spectrum of the primary displays a Zeeman effect indicating a magnetic field with a strength ranging from −94 to 677 G. [6] The visible companion, component B, has a visual magnitude of 5.27. [3]

References

  1. ^ a b c d e f 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.
  2. ^ a b c d Cousins, A. W. J. (1973), "Revised zero points and UBV photometry of stars in the Harvard E and F regions", Memoirs of the Royal Astronomical Society, 77: 223–236, Bibcode: 1973MmRAS..77..223C.
  3. ^ a b c d e Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv: 0806.2878, Bibcode: 2008MNRAS.389..869E, doi: 10.1111/j.1365-2966.2008.13596.x, S2CID  14878976.
  4. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv: 1208.3048, Bibcode: 2012A&A...546A..61D, doi: 10.1051/0004-6361/201219219, S2CID  59451347, A61.
  5. ^ a b c d e f Petit, V.; et al. (February 2013), "A magnetic confinement versus rotation classification of massive-star magnetospheres" (PDF), Monthly Notices of the Royal Astronomical Society, 429 (1): 398–422, arXiv: 1211.0282, Bibcode: 2013MNRAS.429..398P, doi: 10.1093/mnras/sts344.
  6. ^ a b c d e Alecian, E.; et al. (December 2011), "First HARPSpol discoveries of magnetic fields in massive stars", Astronomy & Astrophysics, 536: 4, arXiv: 1111.3433, Bibcode: 2011A&A...536L...6A, doi: 10.1051/0004-6361/201118354, S2CID  51173988, L6.
  7. ^ "omi Lup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-10.
  8. ^ a b Chen, Christine H.; et al. (September 2012), "A Spitzer MIPS Study of 2.5-2.0 M Stars in Scorpius–Centaurus", The Astrophysical Journal, 756 (2): 24, arXiv: 1207.3415, Bibcode: 2012ApJ...756..133C, doi: 10.1088/0004-637X/756/2/133, S2CID  119278056, 133.

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