HD 136138

Last updated
HD 136138
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Serpens
Right ascension 15h 18m 24.507s [1]
Declination +20° 34′ 21.95″ [1]
Apparent magnitude  (V)5.68 [2] + 15.3 [3]
Characteristics
Evolutionary stage Horizontal branch + white dwarf
Spectral type G8IIIa [4] + DA1.7 [3]
B−V color index 0.972±0.004 [2]
Variable type Constant [5] [6]
Astrometry
Radial velocity (Rv)−7.74±0.07 [2]  km/s
Proper motion (μ)RA: −12.993  mas/yr [1]
Dec.: −22.380  mas/yr [1]
Parallax (π)7.7902 ± 0.2193  mas [1]
Distance 420 ± 10  ly
(128 ± 4  pc)
Absolute magnitude  (MV)0.65±0.15 [7]
Orbit [7]
Period (P)506.45±0.18 d
Semi-major axis (a)4.14±0.52"
(≥ 41.76±0.34 Gm [5] )
Eccentricity (e)0.3353±0.0056
Inclination (i)42.9±6.7°
Longitude of the node (Ω)207.0±7.4°
Periastron epoch (T)2,453,240.3±1.3  MJD
Argument of periastron (ω)
(secondary)		35.0±1.4°
Semi-amplitude (K1)
(primary)		6.340±0.044 km/s
Details [7]
A
Mass 1.84±0.40  M☉
Radius 10.3  R☉
Luminosity 56.2  L☉
Surface gravity (log g)2.68  cgs
Temperature 4,960±100  K
Metallicity [Fe/H]−0.08±0.09 [8]   dex
Age 1.45  Gyr
B
Mass 0.59±0.12 or 0.79±0.09  M☉
Surface gravity (log g)8.25±0.15  cgs
Temperature 30,400±780  K
Other designations
BD+21°2755, FK5  1400, GC  20575, HD  136138, HIP  74896, HR  5692, SAO  83755, [9] WD 1516+207 [3]
Database references
SIMBAD data

HD 136138, or HR 5692, is a binary star system in the Serpens Caput segment of the Serpens constellation. It has a golden hue like the Sun and is dimly visible to the naked eye with an apparent visual magnitude of 5.68; [2] the light contribution from the companion is effectively negligible. [8] This system is located at a distance of approximately 420  light years from the Sun based on parallax. [1] It is drifting closer with a radial velocity of −7.7 km/s [2] and has a proper motion of 23.5  mas ·yr−1. [8]

The radial velocity variation of this star was reported by J. R. de Medeiros and M. Mayor in 1999, [5] and it was confirmed as a binary by A. Frankowski and colleagues in 2007 using proper motion measurements. [3] It is an unresolved, single-lined spectroscopic binary system with an orbital period of 1.39 years and an eccentricity (ovalness) of 0.335. Proper motion measurements allow an estimate of the orbital inclination angle as ~43°. [7] Their semimajor axis is around 2.0  AU , or double the distance from the Earth to the Sun. [8]

The stellar classification of the primary component is G8IIIa, [4] indicating this is a evolved G-type giant star that has exhausted the supply of hydrogen at its core. It is a red clump giant that is generating energy through core helium fusion. There is some ambiguous evidence for this being a mild barium star [7] of class Ba0.3, [8] with the spectra showing marginal overabundances of s-process elements. [8] A low level of X-ray emission has been detected, which appears to be coming from the star's corona. [6]

The high level of ultraviolet flux coming from this system strongly suggests the companion is a compact white dwarf. Mass estimates put it in the range of 0.6 to 0.8 times the mass of the Sun, and the temperature is around 30,400 K. [7] It is possible that the earlier evolution of this component contaminated its partner with s-process elements, although the resulting interaction should have circularized the orbit to some degree. [5] The dwarf has a visual magnitude of 15.3 and a hydrogen-dominated atmospheric class of DA1.7. [3]

Related Research Articles

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<span class="mw-page-title-main">Lambda Serpentis</span> Star in the constellation Serpens

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<span class="mw-page-title-main">CD-73°375</span> Binary star in the constellation Volans

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HR 3831, also known as HD 83368, is a binary star system in the southern constellation of Vela at a distance of 233 light years. This object is barely visible to the naked eye as a dim, blue star with an apparent visual magnitude of 6.232. It is approaching the Earth with a heliocentric radial velocity of 4.0±0.3 km/s.

HR 4098, also known as HD 90508, is a binary star system in the northern constellation of Ursa Major at a distance of 75 light years. This object is barely visible to the naked eye as a dim, yellow star with an apparent visual magnitude of 6.45. It is approaching the Earth with a heliocentric radial velocity of 7.2±0.2 km/s.

HD 72945 and HD 72946 form a co-moving star system in the northern constellation of Cancer. HD 72945 is a binary star that is dimly visible to the naked eye as a point of light with an apparent visual magnitude of 5.91. At an angular separation of 10.10″ is the fainter companion star HD 72946 at magnitude 7.25. It is being orbited by a brown dwarf. The system as a whole is located at a distance of approximately 84 light years from the Sun based on parallax measurements.

References

  1. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 4 5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID   119257644.
  3. 1 2 3 4 5 Holberg, J. B.; et al. (2013). "Where are all the Sirius-like binary systems?". Monthly Notices of the Royal Astronomical Society. 435 (3): 2077. arXiv: 1307.8047 . Bibcode:2013MNRAS.435.2077H. doi:10.1093/mnras/stt1433.
  4. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  5. 1 2 3 4 Griffin, R. F. (February 2009). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 204: HR 738, HR 831, HR 5692, and HR 7252". The Observatory. 129: 6–28. Bibcode:2009Obs...129....6G.
  6. 1 2 Jorissen, A.; et al. (February 1996). "New X-ray sources detected among mild barium and S stars". Astronomy and Astrophysics. 306: 467. Bibcode:1996A&A...306..467J.
  7. 1 2 3 4 5 6 Stefanik, Robert P.; et al. (May 2011). "Observations and Orbital Analysis of the Giant White Dwarf Binary System HR 5692". The Astronomical Journal. 141 (5): 9. Bibcode:2011AJ....141..144S. doi:10.1088/0004-6256/141/5/144. S2CID   56137377. 144.
  8. 1 2 3 4 5 6 Merle, T.; et al. (February 2016). "To Ba or not to Ba: Enrichment in s-process elements in binary systems with WD companions of various masses". Astronomy & Astrophysics. 586: 16. arXiv: 1510.05908 . Bibcode:2016A&A...586A.151M. doi:10.1051/0004-6361/201526944. S2CID   119224869. A151.
  9. ↑ "HD 136138". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-12-22.{{cite web}}: CS1 maint: postscript (link)
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