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  mas [1]
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

Xi Boötis, Latinised from ξ Boötis, is a binary star system located at a distance of 22 light-years away from Earth. It is the nearest visible star in the constellation Boötes. The brighter, primary component of the pair has a visual magnitude of 4.70, making it visible to the naked eye.

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.

<span class="mw-page-title-main">Epsilon Serpentis</span> Am star in the constellation Serpens

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.

<span class="mw-page-title-main">Iota Serpentis</span> 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.

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

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 222 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.

<span class="mw-page-title-main">Psi Velorum</span> Binary star in the constellation Vela

Psi Velorum, Latinized from ψ Velorum, is a binary star system in the southern constellation of Vela. Based upon an annual parallax shift of 53.15 mas as seen from Earth, it is located 61.4 light years from the Sun. It is visible to the naked eye with a combined apparent visual magnitude of +3.58. The motion of this system through space makes it a candidate member of the Castor stellar kinematic group.

<span class="mw-page-title-main">Zeta Boötis</span> Star in the constellation Boötis

Zeta Boötis, Latinized from ζ Boötis, is a binary star system in the constellation of Boötes. They have the Flamsteed designation 30 Boötis; Zeta Boötis is the Bayer designation. This system is visible to the naked eye with a combined apparent magnitude of +3.78. The individual magnitudes differ slightly, with component A having a magnitude of 4.46 and component B at the slightly dimmer magnitude 4.55. It is located at a distance of approximately 180 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s.

66 Andromedae is a binary star system in the northern constellation of Andromeda, near the northern border with Perseus. The designation is from the star catalogue of English astronomer John Flamsteed, first published in 1712. It has a combined apparent magnitude of 6.16, which is near the lower limit of stars that are visible to the naked eye under good seeing conditions. An annual parallax shift of 18.3 mas provides a distance estimate of 178 light years. The net radial velocity of the system is poorly constrained, but the pair appear to be moving closer to the Earth with a heliocentric radial velocity of around −5 km/s.

<span class="mw-page-title-main">Sigma Boötis</span> Star in the constellation Boötes

Sigma Boötis, its name Latinized from σ Boötis, is a single star in the northern constellation of Boötes. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude of 4.46. Located to the southeast of Rho Boötis, the dwarf Sigma may at first appear as a naked-eye double, but the angular proximity with Rho is merely line-of-sight. Sigma Boötis is located at a distance of 51.1 light years from the Sun based on parallax. The star has a relatively high proper motion and is traversing the sky at the rate of 0.230″ yr−1.

Chi Boötis, Latinised as χ Boötis, is a single, white-hued star in the northern constellation Boötes, near the eastern constellation border with Corona Borealis. It is faintly visible to the naked eye with an apparent visual magnitude of +5.3. Based upon an annual parallax shift of 13.0 mas as seen from the Earth, it is located about 251 light-years from the Sun. The star is moving closer to the Sun with a radial velocity of −16 km/s.

18 Boötis is a single star in the northern constellation of Boötes, located about 85 light years away from the Sun. It is visible to the naked eye as a faint, yellow-white hued star with an apparent visual magnitude of 5.41. This object is a suspected member of the Ursa Major Moving Group, based on velocity criteria. It has a magnitude 10.84 optical companion at an angular separation of 163.7″ along a position angle of 219°, as of 2010.

50 Cancri is a single star in the zodiac constellation of Cancer, located 183 light years away from the Sun. It has the Bayer designation A2 Cancri; 50 Cancri is the Flamsteed designation. It is faintly visible to the naked eye as a white-hued star with an apparent visual magnitude of 5.89. The star is moving away from the Earth with a heliocentric radial velocity of 23 km/s, having come to within 118 light-years some 1.2 million years ago.

<span class="mw-page-title-main">Chi Capricorni</span> Star in the constellation Capricornus

Chi Capricorni, Latinized from χ Capricorni, is a star in the southern constellation of Capricornus. Based upon an annual parallax shift of 18.14 mas as seen from the Earth, the star is located about 180 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of +5.28.

HD 176051 is a spectroscopic binary star system approximately 49 light years away from Earth in the constellation Lyra. The pair orbit with a period of 22,423 days and an eccentricity of 0.25. Compared to the Sun, they have a somewhat lower proportion of elements more massive than helium. Their individual masses are estimated at 1.07 and 0.71 solar masses (M☉). The system is moving closer to the Sun with a radial velocity of −47 km/s and will reach perihelion in about 269,000 years when it comes within roughly 17 ly (5.1 pc) of 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 108 parsecs (350 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.

HD 118889 is a binary star system in the northern constellation of Boötes. It is faintly visible to the naked eye as a point of light with an apparent visual magnitude of 5.57. The system is located at a distance of approximately 196 light years from the Sun based on stellar parallax, but is drifting closer with a radial velocity of −26 km/s.

HD 134064 is a binary star system in the northern constellation of Boötes. It is faintly visible to the naked eye with a combined apparent visual magnitude of 6.03. This system is located at a distance of 247 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of –7.0 km/s.

<span class="mw-page-title-main">Zeta Sagittae</span> Star in the constellation Sagitta

Zeta Sagittae (ζ Sagittae) is triple star system in the northern constellation of Sagitta. It is visible to the naked eye, having a combined apparent visual magnitude of +5.00. Based upon an annual parallax shift of 12.79 mas, the distance to this star is approximately 260 light years.

<span class="mw-page-title-main">Gamma Crateris</span> 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.

References

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  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.
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  10. ↑ Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy & Astrophysics. 367 (Third ed.): 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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