25 Serpentis

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This article is about A2 Serpentis. For other stars with this Bayer designation, see A Serpentis.
25 Serpentis
Serpens constellation map.svg
Red circle.svg

Location of 25 Serpentis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Serpens
Right ascension 15h 46m 05.63636s[1]
Declination −01° 48′ 15.0830″[1]
Apparent magnitude (V) 5.37 - 5.40[2]
Characteristics
Spectral type B8IV/V[3]
U−B color index −0.40[4]
B−V color index −0.05[4]
Variable type SPB[5]
Astrometry
Radial velocity (Rv) −9.50 ± 0.3[6] km/s
Proper motion (μ) RA: −23.15[1] mas/yr
Dec.: −30.50[1] mas/yr
Parallax (π) 7.25 ± 0.31[1] mas
Distance 450 ± 20 ly
(138 ± 6 pc)
Orbit[7]
Period (P) 38.927 ± 0.004
Eccentricity (e) 0.731 ± 0.006
Periastron epoch (T) 2450132.80 ± 0.06
Argument of periastron (ω)
(secondary)
201.8 ± 0.8°
Semi-amplitude (K1)
(primary)
43.1 ± 0.7 km/s
Semi-amplitude (K2)
(secondary)
86 ± 1 km/s
Other designations
25 Ser, PT Ser, HD 140873, HIP 77227, HR 5863, SAO 140740, BD−01° 3092
Database references
SIMBAD data

25 Serpentis is a star system in the constellation of Serpens Caput. With an apparent magnitude of 5.37, it is just barely visible to the naked eye. The system is estimated to be some 450 light-years (138 parsecs) based on its parallax.[1]

25 Serpentis is a spectroscopic binary,[8] meaning that the individual components are too close to be resolved, but periodic Doppler shifts in their spectra indicate orbital motion. The system consists of a hot B-type giant and an A-type main-sequence star. The two stars orbit each other every 38.9 days, and have a very eccentric orbit, with an orbital eccentricity of 0.731.[7] The primary is a slowly pulsating B-type star, which causes the system to vary by 0.03 magnitudes;[2] for that reason it has been given the variable star designation PT Serpentis.

References[edit]

  1. ^ a b c d e f van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b VSX; Otero, S. A (10 February 2012). "PT Serpentis". AAVSO Website. American Association of Variable Star Observers. Retrieved 28 May 2014. 
  3. ^ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars, Vol. 5". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H. 
  4. ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Bibcode:1986EgUBV........0M. 
  5. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S. 
  6. ^ Pourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573Freely accessible. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. 
  7. ^ a b De Cat, P.; et al. (2000). "A study of bright southern slowly pulsating B stars. I. Determination of the orbital parameters and of the main frequency of the spectroscopic binaries". Astronomy and Astrophysics. 355: 1015–1030. Bibcode:2000A&A...355.1015D. 
  8. ^ Petrie, R. M.; Phibbs, E. (1950). "Redetermination of the spectrographic orbits of iot Peg and 25 Ser.". Publications of the Dominion Astrophysical Observatory Victoria. 8: 225. Bibcode:1950PDAO....8..225P.