Omicron Lupi

Short description: Binary star system in the constellation Lupus

Omicron Lupi

Location of ο Lupi (circled in red)

Observation data
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[1] mas
Distance| 400 ± 30 ly
(124 ± 9 pc)
Absolute magnitude (MV)| −1.2±0.3[5]
Details
Mass| 5.7±0.2[5] M☉
Radius| 3.5[5] R☉
Luminosity| 1,260[5] L☉
Surface gravity (log g)| 4.1±0.1[5] cgs
Temperature| 18,000[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. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
2. ↑ 2.0 2.1 2.2 2.3 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. ↑ 3.0 3.1 3.2 3.3 3.4 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Petit, V. et al. (February 2013), "A magnetic confinement versus rotation classification of massive-star magnetospheres", Monthly Notices of the Royal Astronomical Society 429 (1): 398–422, doi:10.1093/mnras/sts344, Bibcode: 2013MNRAS.429..398P, https://pure.uva.nl/ws/files/1746728/147519_A_magnetic_confinement.pdf.
6. ↑ 6.0 6.1 6.2 6.3 6.4 Alecian, E. et al. (December 2011), "First HARPSpol discoveries of magnetic fields in massive stars", Astronomy & Astrophysics 536: 4, doi:10.1051/0004-6361/201118354, L6, Bibcode: 2011A&A...536L...6A.
7. ↑ "omi Lup". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Lup.
8. ↑ 8.0 8.1 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, doi:10.1088/0004-637X/756/2/133, 133, Bibcode: 2012ApJ...756..133C.

* v
* t
* e

Stars of Lupus

Bayer|

* α
* β
* γ
* δ
* ε
* ζ
* η
* θ
* ι
* κ1
* κ2
* λ
* μ
* ν1
* ν2
* ξ1
* ξ2
* ο
* π
* ρ
* σ
* τ1
* τ2
* υ
* φ1
* φ2
* χ
* ψ1
* ψ2
* ω

Flamsteed|

* 1 (i)
* 2 (f)

Variable|

* RU
* RY
* BR
* EX
* FT
* FW
* GG
* GM
* GQ
* HR
* HX
* HZ
* II
* IM
* KT (d)
* NY
* NZ

HR|

* 5362
* 5364
* 5377
* 5380
* 5401
* 5412
* 5413
* 5426
* 5427
* 5444
* 5450 (a)
* 5457
* 5458
* 5494
* 5495 (b)
* 5498
* 5509
* 5556 (c)
* 5559
* 5566
* 5580
* 5595
* 5607
* 5615
* 5617
* 5625
* 5636
* 5637
* 5642
* 5650
* 5651 (e)
* 5653
* 5663
* 5667
* 5668
* 5682
* 5688
* 5689
* 5696
* 5724 (k)
* 5736
* 5738
* 5742
* 5751
* 5753
* 5767
* 5773
* 5784
* 5790
* 5807
* 5821
* 5822
* 5825 (g)
* 5837 (h)
* 5846
* 5860
* 5862
* 5864
* 5893
* 5916
* 5918
* 5923
* 5929
* 5935
* 5943
* 5952
* 5956
* 5967
* 5970
* 5974
* 5975
* 5991

HD|

* 125809
* 126093
* 126525
* 126759
* 128154
* 129624
* 133399
* 133469
* 133518
* 135430
* 135468
* 136607
* 137785
* 137919
* 138395
* 142527

Gliese|

* Gliese 588

Other|

* He 2-113
* HIP 70849
* Lupus-TR-3
* SAO 206462
* SSSPM J1549-3544
* 4U 1543-47

* List

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