Binary star system in the constellation Puppis
This article is about l Puppis and is not to be confused with
j Puppis or
L Puppis .
3 Puppis Location of 3 Puppis (circled)
Observation dataEpoch J2000 Equinox J2000 Constellation Puppis Right ascension 07h 43m 48.46872s [ 1] Declination −28° 57′ 17.3720″[ 1] Apparent magnitude (V)3.93[ 2] Characteristics Spectral type A2.7Ib[ 2] (A2Ia - A3IIpe[ 3] Apparent magnitude (K)2.340[ 4] U−Bcolor index −0.09[ 5] B−Vcolor index +0.18[ 5] Astrometry Radial velocity (Rv )± 2.0[ 6] km/s Proper motion (μ)RA: mas /yr [ 1] Dec.: mas /yr [ 1] Parallax (π)0.59± 0.17 mas [ 1] Distance ± 280ly ± 85pc )[ 6] Absolute magnitude (MV )−5.5[ 2] Orbit [ 6] Primary A Companion B Period (P)± 0.1Semi-major axis (a)± 0.03 AU Semi-amplitude 1 )± 0.8Details[ 6] A Mass ± 0.5M ☉ Radius ± 7R ☉ Luminosity +3,300 L ☉ Surface gravity (log g )± 0.1cgs Temperature ± 500K Rotational velocity (v sin i )± 5B Mass ± 0.25M ☉ Radius 0.3 R ☉ Surface gravity (log g )5.0 cgs Temperature 50,000 K Other designations l Puppis,GSC 06552-03228,HD 62623,HIP 37677,HR 2996,SAO 174400,CD −28°4774Database references SIMBAD data
3 Puppis (3 Pup ) is aspectroscopic binary in theconstellation Puppis . It is a very rare A[e] supergiant, referred to as aB[e] star despite its spectral classification, and itsapparent magnitude is 3.93.
3 Puppis is surrounded by a disc of circumstellar dust, which is unusual for an A-type star.[ 3] subdwarf that is transferring mass to the supergiant. Due to mass transfer, its mass reduced from 3.6 M ☉ when it formed to the current 0.75 M ☉ .[ 6] [ a] stellar wind by the companion allows the dust to form unusually close to such a luminous star.[ 3]
^ Calculated from rotational velocity divided by critical velocity, 35/178 = 0.20. ^a b c d 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 . ^a b c Klochkova, V. G.; Sendzikas, E. G.; Chentsov, E. L. (2015). "Spectral atlas of A-type supergiants".Astrophysical Bulletin .70 (1):99– 108.arXiv :1502.01444 Bibcode :2015AstBu..70...99K .doi :10.1134/S1990341315010113 .S2CID 119229144 . ^a b c Meilland, A.; Kanaan, S.; Borges Fernandes, M.; Chesneau, O.; Millour, F.; Stee, Ph.; Lopez, B. (2010). "Resolving the dusty circumstellar environment of the A[e] supergiant HD 62623 with the VLTI/MIDI".Astronomy and Astrophysics .512 : A73.arXiv :0912.1954 Bibcode :2010A&A...512A..73M .doi :10.1051/0004-6361/200913640 .S2CID 119225591 . ^ Kraus, M.; Oksala, M. E.; Cidale, L. S.; Arias, M. L.; Torres, A. F.; Borges Fernandes, M. (2015). "Discovery of SiO Band Emission from Galactic B[e] Supergiants".The Astrophysical Journal Letters .800 (2): L20.arXiv :1501.07063 Bibcode :2015ApJ...800L..20K .doi :10.1088/2041-8205/800/2/L20 .S2CID 118847782 . ^a b Gutierrez-Moreno, A.; Moreno, H.; Loyola, P.; Cortes, G. (1986). "Low dispersion spectrophotometry of bright early-type stars".Astronomy and Astrophysics Supplement Series .64 : 205.Bibcode :1986A&AS...64..205G . ^a b c d e Miroshnichenko, A. S.; Danford, S.; Zharikov, S. V.; Klochkova, V. G.; Chentsov, E. L.; Vanbeveren, D.; Zakhozhay, O. V.; Manset, N.; Pogodin, M. A.; Omarov, C. T.; Kuratova, A. K.; Khokhlov, S. A. (July 2020)."Properties of Galactic B[e] Supergiants. V. 3 Pup–Constraining the Orbital Parameters and Modeling the Circumstellar Environments" .The Astrophysical Journal .897 (1): 48.arXiv :2005.07754 Bibcode :2020ApJ...897...48M .doi :10.3847/1538-4357/ab93d9 ISSN 0004-637X .
