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Delta Lupi

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δ Lupi
Location of δ Lupi (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Lupus
Right ascension 15h 21m 22.32168s[1]
Declination −40° 38′ 51.0738″[1]
Apparent magnitude (V) 3.20 - 3.24[2]
Characteristics
Spectral type B1.5 IV[3]
U−B color index −0.910[4]
B−V color index −0.224[4]
Variable type β Cep[5][2]
Astrometry
Radial velocity (Rv)+0.2[6] km/s
Proper motion (μ) RA: −19.49[1] mas/yr
Dec.: −25.29[1] mas/yr
Parallax (π)3.69 ± 0.54 mas[1]
Distanceapprox. 900 ly
(approx. 270 pc)
Absolute magnitude (MV)−3.1[7]
Details
Mass11.9±0.2[8] M☉
Radius6.1[9] R☉
Luminosity10,000[8] L☉
Surface gravity (log g)3.86[8] cgs
Temperature22,908[8] K
Metallicity [Fe/H]−0.25±0.11[10] dex
Rotational velocity (v sin i)230[11] km/s
Age15.4±1.3[8] Myr
Other designations
CD−40°9538, FK5 1402, HD 136298, HIP 75141, HR 5695, SAO 225691, UBV 13201.[12]
Database references
SIMBADdata

Delta Lupi (δ Lupi, δ Lup) is a star in the southern circumpolar constellation of Lupus. In traditional Chinese astronomy, it is "the 2nd (star) of the Cavalry Officer" (騎官二). With an apparent visual magnitude of 3.2, it is the fourth-brightest star in the constellation. The distance to this star has been measured using the parallax technique, yielding an estimate of roughly 900 light-years with a 15% margin of error.[1]

A light curve for Delta Lupi, plotted from TESS data[13]

The spectrum of this star matches a stellar classification of B1.5 IV,[3] which indicates this star has entered the subgiant stage and is in the process of evolving into a giant star. It is radiating around 10,000 times the luminosity of the Sun from its outer atmosphere at an effective temperature of 23,000 K, giving it a blue-white hue. This star has nearly 12 times the mass of the Sun and is roughly 15 million years old.[8]

Delta Lupi is a Beta Cephei variable star that undergoes periodic pulsations. It has a single period of variability lasting 0.1655 days, or six cycles per day.[5] This is a proper motion member of the Upper Centaurus–Lupus sub-group in the Scorpius–Centaurus OB association, the nearest such co-moving association of massive stars to the Sun.[7]

See also

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References

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  1. ^ a b c d e f van Leeuwen, F. (November 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 Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. ISSN 1063-7729. S2CID 255195566.
  3. ^ a b Hiltner, W. A.; Garrison, R. F.; Schild, R. E. (July 1969), "MK spectral types for bright southern OB stars", Astrophysical Journal, 157: 313, Bibcode:1969ApJ...157..313H, doi:10.1086/150069
  4. ^ a b Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168
  5. ^ a b Smolec, R.; Moskalik, P. (May 2007), "Amplitude saturation in β Cephei models", Monthly Notices of the Royal Astronomical Society, 377 (2): 645–656, arXiv:astro-ph/0702406, Bibcode:2007MNRAS.377..645S, doi:10.1111/j.1365-2966.2007.11620.x, S2CID 17908442
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications. IAU Symposium no. 30. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ a b de Geus, E. J.; de Zeeuw, P. T.; Lub, J. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61, Bibcode:1989A&A...216...44D
  8. ^ a b c d e f Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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
  9. ^ Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189 (3): 601–605, Bibcode:1979MNRAS.189..601U, doi:10.1093/mnras/189.3.601
  10. ^ Niemczura, E.; Daszyńska-Daszkiewicz, J. (April 2005), "Metallicities of the β Cephei stars from low-resolution ultraviolet spectra", Astronomy and Astrophysics, 433 (2): 659–669, arXiv:astro-ph/0410440, Bibcode:2005A&A...433..659N, doi:10.1051/0004-6361:20040396, S2CID 14295631. Note: value taken from [m/H].
  11. ^ Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1): 1. Bibcode:1970CoAsi.239....1B.
  12. ^ "del Lup". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2007-01-18.
  13. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 11 December 2022.
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