36 Serpentis

Last updated
36 Serpentis
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Serpens
Right ascension 15h 51m 15.59418s [1]
Declination −03° 05′ 25.7938″ [1]
Apparent magnitude  (V)5.09 [2] (5.2 + 7.8) [3]
Characteristics
Spectral type A3Vn [4] or A2IV-Vn [5] (A7 + G0) [6]
U−B color index +0.07 [7]
B−V color index +0.12 [7]
Astrometry
Radial velocity (Rv)−8 [8]  km/s
Proper motion (μ)RA: −91.09 [1]   mas/yr
Dec.: −28.21 [1]   mas/yr
Parallax (π)20.10 ± 0.33 [1]   mas
Distance 162 ± 3  ly
(49.8 ± 0.8  pc)
Absolute magnitude  (MV)1.61 [2]
Orbit [6]
Period (P)50.6±1.5 yr
Semi-major axis (a)0.400±0.006″
Eccentricity (e)0.8323±0.0047
Inclination (i)98.08±0.31°
Longitude of the node (Ω)74.00±0.31°
Periastron epoch (T)2002.78±0.17
Argument of periastron (ω)
(secondary)		72.84±0.91°
Details
36 Ser A
Mass 2.04 [9]   M☉
Radius 1.65 [10]   R☉
Luminosity 19.13 [2]   L☉
Surface gravity (log g)3.89 [11]   cgs
Temperature 8246 [11]   K
Metallicity [Fe/H]−2.00 [11]   dex
Rotational velocity (v sin i)229 [12]  km/s
Age 723 [9]   Myr
Other designations
b Ser, 36 Ser, BD−02°4058, FK5  2249, GC  4210, HD  141851, HIP  77660, HR  5895, SAO  140801, WDS J15513-0305 [13]
Database references
SIMBAD data

36 Serpentis is a binary star [14] system in the equatorial constellation of Serpens. It has the Bayer designation b Serpentis, while 36 Serpentis is the Flamsteed designation. [13] The system is visible to the naked eye as a dim, white-hued point of light with a combined apparent visual magnitude of 5.09. [2] It is located 162  light years away from the Sun based on parallax, [1] and is moving closer with a radial velocity of −8 km/s. [8]

This is a spectroscopic binary star system with a long orbital period of 52.8 years and a high eccentricity of 0.83. The combined mass of the pair is 3.09±0.28  M☉ . [6] Gray et al. (2017) found a merged stellar classification of A2IV-Vn for this system, [5] while Cowley et al. matched it with a class of A3Vn, [4] where the 'n' indicates "nebulous" lines caused by rapid rotation.

The primary component is a Lambda Boötis star, meaning that it has solar-like amounts of carbon, nitrogen, and oxygen, while containing very low amounts of iron peak elements. [15] It is an A7 [6] class main sequence star of visual magnitude 5.2 [3] that is spinning rapidly, showing a projected rotational velocity of 229. [12] The star is 723 [9]  million years old with around double the mass of the Sun. It is radiating 19 [2] times the Sun's luminosity from its photosphere at an effective temperature of 8,246 K. [11]

The cooler secondary component, a G0 star, [6] is the source for the X-ray emission that has been detected coming from this system. [6] It has a visual magnitude of 7.8. [3]

Related Research Articles

Kappa<sup>1</sup> Sagittarii Star in the constellation Sagittarius

Kappa1 Sagittarii (κ1 Sagittarii) is a solitary, white-hued star in the zodiac constellation of Sagittarius. It has an apparent visual magnitude of +5.58, which is bright enough to be faintly visible to the naked eye. According to the Bortle scale, it can be viewed from dark suburban skies. Based upon an annual parallax shift of 15.12 mas as seen from Earth, this star is located around 223 light years from the Sun. It is advancing in the general direction of the Sun with a radial velocity of −11.6 km/s.

Mu Serpentis, Latinized from μ Serpentis, is a binary star in the Serpens Caput (head) section of the equatorial constellation Serpens. It is visible to the naked eye with an apparent visual magnitude of 3.543. Based upon an annual parallax shift of 19.23 mas as seen from Earth, it is located around 170 light years from the Sun.

Xi Serpentis, Latinized from ξ Serpentis, is a triple star system in the Serpens Cauda (tail) section of the equatorial constellation Serpens. Based upon an annual parallax shift of 30.98 mas as seen from Earth, it is located 105.3 light years from the Sun. The star system is visible to the naked eye with a base apparent visual magnitude of +3.54. It is moving closer to the Sun and will make perihelion passage at a distance of 27 ly (8.2 pc) in around 690,000 years.

Epsilon Serpentis, Latinized from ε Serpentis, is a single, white-hued star in the constellation Serpens, in its head. It is visible to the naked eye with an apparent visual magnitude of +3.69. Based upon an annual parallax shift of 46.30 mas as seen from Earth, it is located 70 light years from the Sun. It is moving closer to the Sun with a radial velocity of −9 km/s.

Omicron Serpentis is a solitary star in the Serpens Cauda (tail) section of the equatorial constellation Serpens. Based upon an annual parallax shift of 18.83 mas as seen from Earth, it is located around 173 light years from the Sun. The star is visible to the naked eye with a base apparent visual magnitude of +4.26.

Iota Serpentis Star in the constellation Serpens

ι Serpentis, Latinized as Iota Serpentis and abbreviated Iot Ser, is a triple star system in the constellation Serpens, in its head. It is approximately 190 light years from Earth.

Pi Serpentis, Latinized from π Serpentis, is a solitary white-hued star in the constellation Serpens, located in its head, Serpens Caput. Based upon an annual parallax shift of 18.22 mas as seen from Earth, it is located around 179 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.82.

Chi Serpentis is a solitary star in the Serpens Caput section of the equatorial constellation Serpens. Based upon an annual parallax shift of 14.84 mas as seen from Earth, it is located around 220 light years from the Sun. The star is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of +5.30.

Upsilon Serpentis, Latinized from υ Serpentis, is a star in the Serpens Caput section of the constellation Serpens. Based upon an annual parallax shift of 13.04 mas as seen from Earth, it is located around 250 light years from the Sun. The star is bright enough to be faintly visible to the naked eye, having an apparent visual magnitude of +5.70. It is a member of the Hyades group, a stream of stars that share a similar trajectory to the Hyades cluster.

Psi Serpentis is a triple star system within the Serpens Caput part of the equatorial constellation Serpens. Based upon an annual parallax shift of 68.22 mas as seen from Earth, it is located approximately 47.8 light years from the Sun. This system came closest approach to the Sun about 585,000 years ago when it made perihelion passage at an estimated distance of 23.27 ly (7.134 pc). Psi Serpentis is faintly visible to the naked eye with an apparent visual magnitude of 5.84.

Sigma Tauri

Sigma Tauri is the Bayer designation for a pair of white-hued stars in the zodiac constellation of Taurus. The system is a visual double star, whose components are designated σ1 Tauri and σ2 Tauri, with the latter being the more northerly star. The two are separated by 7.2 arcminutes on the sky and can be readily split with a pair of binoculars. They have apparent visual magnitudes of +5.07 and +4.70, respectively, which indicated they are both visible to the naked eye. Based upon parallax measurements, σ1 Tauri is about 147 light years from the Sun, while σ2 Tauri is 156 light years distant.

5 Aquilae is a quadruple star system in the constellation of Aquila. 5 Aquilae is the Flamsteed designation. The combined apparent visual magnitude of the system is 5.9, which means it is faintly visible to the naked eye. With an annual parallax shift of 8.94 mas, the distance to this system is estimated as approximately 360 light-years, albeit with a 13% margin of error.

38 Boötis is a single star in the northern constellation of Boötes, located approximately 157 light years from the Sun. It has the traditional name Merga and the Bayer designation h Boötis; 38 Boötis is the star's Flamsteed designation. This object is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of 5.76. It is moving closer to the Earth with a heliocentric radial velocity of −4.5 km/s.

Pi Cassiopeiae Variable star in the constellation Cassiopeia

Pi Cassiopeiae, Latinized from π Cassiopeiae, is a close binary star system in the constellation Cassiopeia. It is visible to the naked eye with an apparent visual magnitude of +4.949. Based upon an annual parallax shift of 18.63 mas as seen from Earth, this system is located about 175 light years from the Sun.

HD 6114 is a visual binary star system in the northern constellation of Andromeda. With a combined apparent magnitude of 6.46, the star can only be seen with the naked eye by keen-eyed observers even on the best of nights. Based upon an annual parallax shift of 10.4 mas as seen from Earth's orbit, the system is located approximately 96 parsecs (310 ly) distant.

45 Aquilae, abbreviated 45 Aql, is a triple star system in the equatorial constellation of Aquila. 45 Aquilae is its Flamsteed designation. It is located 350 light-years away from Earth, give or take a 6 light-year margin of error, and has a combined apparent visual magnitude of 5.7. The system is moving closer to the Earth with a heliocentric radial velocity of -46 km/s.

Gamma Crateris Star in the constellation Crater

Gamma Crateris is a binary star system, divisible with a small amateur telescope, and located at the center of the southern constellation of Crater. It is visible to the naked eye with an apparent visual magnitude of 4.06. With an annual parallax shift of 39.62 mas as seen from Earth, this star is located 82.3 light years from the Sun. Based upon the motion of this system through space, it is a potential member of the Castor Moving Group.

30 Monocerotis is a single star in the equatorial constellation of Hydra, located 122 light years away from the Sun. It has the Bayer designation C Hydrae; 30 Monocerotis is the Flamsteed designation and was assigned when it belonged to the Monoceros constellation. The object is visible to the naked eye as a white-hued star with an apparent visual magnitude of 3.90. It is moving away from the Earth with a heliocentric radial velocity of +10 km/s.

Tau1 Hydrae is a triple star system in the equatorial constellation of Hydra. Based upon the annual parallax shift of the two visible components as seen from Earth, they are located about 18 parsecs (59 ly) from the Sun. The system has a combined apparent visual magnitude of +4.59, which is bright enough to be visible to the naked eye at night.

5 Serpentis is a wide binary star system in Serpens Caput, the western section of the equatorial constellation of Serpens. It is faintly visible to the naked eye with an apparent visual magnitude of 5.10. Based upon an annual parallax shift of 39.40±0.29 mas as viewed from Earth's orbit, it is located 83 light years away. The brighter member is an IAU radial velocity standard star, and it is moving away from the Sun with a heliocentric radial velocity of +54.3 km/s. The system made its closest approach to the Sun about 153,000 years ago at a separation of 68 ly (20.7 pc).

References

  1. 1 2 3 4 5 6 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.
  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 Docobo, José A.; et al. (2010). "EMCCD Speckle Interferometry with the 6 m Telescope: Astrometric Measurements, Differential Photometry, and Orbits". The Astronomical Journal. 140 (4): 1078–1083. Bibcode:2010AJ....140.1078D. doi: 10.1088/0004-6256/140/4/1078 .
  4. 1 2 Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. 1 2 Gray, R. O.; et al. (July 2017). "The Discovery of λ Bootis Stars: The Southern Survey I". The Astronomical Journal. 154 (1): 11. Bibcode:2017AJ....154...31G. doi: 10.3847/1538-3881/aa6d5e . 31.
  6. 1 2 3 4 5 6 Mason, Brian D.; et al. (September 2010). "Binary Star Orbits. IV. Orbits of 18 Southern Interferometric Pairs". The Astronomical Journal. 140 (3): 735–743. Bibcode:2010AJ....140..735M. doi: 10.1088/0004-6256/140/3/735 .
  7. 1 2 Johnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory. 4: 99. Bibcode:1966CoLPL...4...99J.
  8. 1 2 Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Carnegie Institute Washington D.C. Publication. Bibcode:1953GCRV..C......0W.
  9. 1 2 3 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.
  10. ↑ Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy & Astrophysics (Third ed.). 367: 521–24. arXiv: astro-ph/0012289 . Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID   425754.
  11. 1 2 3 4 Prugniel, Ph.; et al. (1986). "The atmospheric parameters and spectral interpolator for the MILES stars". Astronomy & Astrophysics. 531: A165. arXiv: 1104.4952 . Bibcode:2011A&A...531A.165P. doi:10.1051/0004-6361/201116769. S2CID   54940439.
  12. 1 2 Royer, F.; et al. (2007). "Rotational velocities of A-type stars. III. Velocity distributions". Astronomy & Astrophysics. 463 (2): 671–682. arXiv: astro-ph/0610785 . Bibcode:2007A&A...463..671R. doi:10.1051/0004-6361:20065224. S2CID   18475298.
  13. 1 2 "36 Ser". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-07-14.
  14. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  15. ↑ Nikolov, G.; et al. (April 2008). "Spectroscopic orbit determination of two metal-weak dwarf stars: HD64491 and HD141851". Contributions of the Astronomical Observatory Skalnaté Pleso. 38 (2): 433–434. Bibcode:2008CoSka..38..433N.
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