Xi Lupi
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Lupus |
| ξ1 Lup | |
| Right ascension | 15h 56m 53.48964s[1] |
| Declination | −33° 57′ 58.0131″[1] |
| Apparent magnitude (V) | 5.114[2] |
| ξ2 Lup | |
| Right ascension | 15h 56m 54.11281s[3] |
| Declination | −33° 57′ 51.3380″[3] |
| Apparent magnitude (V) | 5.55[4] |
| Characteristics | |
| ξ1 Lup | |
| Spectral type | A3 V[5] |
| U−B color index | 0.069[2] |
| B−V color index | 0.116[2] |
| ξ2 Lup | |
| Spectral type | B9 V[5] |
| B−V color index | +0.06[4] |
| Astrometry | |
| ξ1 Lup | |
| Radial velocity (Rv) | −10.0±4.2[6] km/s |
| Proper motion (μ) | RA: +11.963 mas/yr[1] Dec.: −37.94 mas/yr[1] |
| Parallax (π) | 15.0230±0.1787 mas[1] |
| Distance | 217 ± 3 ly (66.6 ± 0.8 pc) |
| ξ2 Lup | |
| Radial velocity (Rv) | −12.20±1.78[6] km/s |
| Proper motion (μ) | RA: +10.663 mas/yr[3] Dec.: −41.073 mas/yr[3] |
| Parallax (π) | 15.5015±0.0722 mas[3] |
| Distance | 210.4 ± 1.0 ly (64.5 ± 0.3 pc) |
| Details | |
| ξ1 Lup A | |
| Mass | 2.0[7] M☉ |
| Radius | 2.0[7] R☉ |
| Surface gravity (log g) | 4.14±0.14[8] cgs |
| Temperature | 8,650[7] K |
| Rotational velocity (v sin i) | 78[8] km/s |
| Age | 450[7] Myr |
| ξ1 Lup B | |
| Mass | 1.65[7] M☉ |
| Radius | 1.6[7] R☉ |
| Temperature | 7,800[7] K |
| Age | 450[7] Myr |
| ξ2 Lup | |
| Mass | 2[7] M☉ |
| Radius | 1.74±0.04[9] R☉ |
| Luminosity | 22.7±1.0[9] L☉ |
| Surface gravity (log g) | 4.34±0.06[9] cgs |
| Temperature | 9,550±120[9] K |
| Rotational velocity (v sin i) | 184[8] km/s |
| Age | 500[7] Myr |
| Other designations | |
| CCDM J15569-3358, WDS J15569-3358 | |
| A: ξ1 Lup, CD−33°10826A, HD 142629, HIP 78105, HR 5925, SAO 207144[10] | |
| B: ξ2 Lup, CD−33°10826B, HD 142630, HIP 78106, HR 5926, SAO 207145[11] | |
| Database references | |
| SIMBAD | ξ1 Lup |
| ξ2 Lup | |
Xi Lupi is a triple star system[7] in the southern constellation of Lupus. Its main identifier is a Bayer designation that is Latinized from ξ Lupi, and abbreviated Xi Lup or ξ Lup. The combined apparent magnitude is 4.56, making it faintly visible to the naked eye.[a] The system is located at 210 light-years (64 parsecs) from Earth, and is a member of the Upper Scorpius sub-group of the nearby Sco OB2 association.[12]
Characteristics
[edit]This is a hierarchical triple system. It consists on the binary star ξ1 Lup and the star ξ2 Lup; both form a visual binary separated by 10.2" in the sky, or 660 astronomical units at their distance. The components of ξ1 Lup, named ξ1 Lup A and B, are separated by about the same distance Earth is from Sun (1 au), the orbital period is an estimated 200 days, although the observed separation is merely a projected separation and the whole orbit has not been observed.[7]
ξ1 Lup has a combined stellar classification of A3 V,[5] and its primary and secondary components have, respectively, 2.0 and 1.65 times the mass of the Sun, radii 2.0 and 1.6 times solar and effective temperatures of 8,650 and 7,850 K.[7]
ξ2 Lup has a stellar classification of B9 V,[5] matching a B-type main-sequence star. It has twice the mass of the Sun,[7] 1.74 times the Sun's radius, is 23 times more luminous and has an effective temperature of 9,550 K.[9] It spins rapidly with a projected rotational velocity of 184 km/s.[8] The star has a peculiar velocity of 14.3±1.9 km/s relative to its neighbors, and is probably (86% chance) a runaway star.[13]
The system is currently about 500 million years old. When ξ1 Lup A evolves into an AGB star, it will likely engulf component Ab, but given the orbit of the system is unknown, it may be more distant, and survive its companion's AGB phase. Assuming the Aa-Ab separation is correct, the system will likely end as a triple white dwarf system; few of such system have been observed so far.[7]
Notes
[edit]- ^ Calculated from components' individual magnitudes using the equation given in Apparent magnitude § Magnitude addition.
References
[edit]- ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c Slawson, Robert W.; Hill, Robert J.; Landstreet, John D. (September 1992), "A homogeneous catalog of new UBV and H-beta photometry of B- and A-type stars in and around the Scorpius-Centaurus OB association", Astrophysical Journal Supplement Series, 82 (1): 117–144, Bibcode:1992ApJS...82..117S, doi:10.1086/191711.
- ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b Høg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862.
- ^ a b c d Levato, H. (January 1975), "Rotational velocities and spectral types for a sample of binary systems", Astronomy and Astrophysics Supplement Series, 19: 91–99, Bibcode:1975A&AS...19...91L.
- ^ a b 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.
- ^ a b c d e f g h i j k l m n o Waisberg, Idel; Klein, Ygal; Katz, Boaz (July 2025), "Hidden Companions to Intermediate-mass Stars. Upgraded Multiplicity 2 → 3. XXIX. Discovery of a 1.65 M☉, 1.0 au Companion to Xi1 Lupi", Research Notes of the AAS, 9 (7), doi:10.3847/2515-5172/adefd9.
- ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ a b c d e Stassun, Keivan G.; Oelkers, Ryan J.; Paegert, Martin; Torres, Guillermo; Pepper, Joshua; De Lee, Nathan; Collins, Kevin; Latham, David W.; Muirhead, Philip S.; Chittidi, Jay; Rojas-Ayala, Bárbara; Fleming, Scott W.; Rose, Mark E.; Tenenbaum, Peter; Ting, Eric B. (2019-10-01), "The Revised TESS Input Catalog and Candidate Target List", The Astronomical Journal, 158 (4): 138, arXiv:1905.10694, Bibcode:2019AJ....158..138S, doi:10.3847/1538-3881/ab3467, ISSN 0004-6256.
- ^ "ksi01 Lup", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-03-08.
- ^ "ksi02 Lup", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-03-08.
- ^ Brown, A. G. A.; Verschueren, W. (March 1997), "High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2", Astronomy and Astrophysics, 319: 811–838, arXiv:astro-ph/9608089, Bibcode:1997A&A...319..811B.
- ^ Tetzlaff, N.; et al. (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.
