35 Sextantis

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35 Sextantis
Sextans constellation map.svg
Red circle.svg
Location of 35 Sex on the map (circled)
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Sextans
A
Right ascension 10h 43m 20.92086s [1]
Declination +04° 44′ 51.6121″ [1]
Apparent magnitude  (V)6.09±0.01 [2]
B
Right ascension 10h 43m 20.52732s [3]
Declination +04° 44′ 48.2184″ [3]
Apparent magnitude  (V)7.01±0.01 [2]
Characteristics
U−B color index +1.09 [4]
B−V color index +1.17 [4]
A
Spectral type K2.5 III [5]
B
Spectral type K1 II-III [6]
Astrometry
A
Radial velocity (Rv)−3.15±0.16 [7]  km/s
Proper motion (μ)RA: +22.430  mas/yr [1]
Dec.: −33.285  mas/yr [1]
Parallax (π)4.6773 ± 0.1457  mas [1]
Distance 700 ± 20  ly
(214 ± 7  pc)
B
Radial velocity (Rv)−1.49±0.98 [7]  km/s
Proper motion (μ)RA: +24.384  mas/yr [3]
Dec.: −37.384  mas/yr [3]
Parallax (π)4.5442 ± 0.15  mas [3]
Distance 720 ± 20  ly
(220 ± 7  pc)
Orbit [8]
PrimaryA
CompanionB
Period (P)23,302 yr
Semi-major axis (a)6.80"
(1,460  AU )
Orbit [9]
PrimaryBa
CompanionBb
Period (P)1,568.7±2.2  d
Semi-major axis (a)0.021"
(4.64  AU )
Eccentricity (e)0.388±0.057
Periastron epoch (T)2,451,911±27  JD
Argument of periastron (ω)
(secondary)		311.8±3.3°
Semi-amplitude (K1)
(primary)		5.55±0.15 km/s
Details
A
Mass 2.45 [8]   M☉
Radius 25.39+0.8
−2.2 [10]   R☉
Luminosity 240±7 [10]   L☉
Temperature 4,512±122 [11]   K
Metallicity [Fe/H]−0.17 [12]   dex
Rotational velocity (v sin i)3.7±0.3 [7]  km/s
Ba
Mass 2.44 [8]   M☉
Radius 10.15+0.34
−0.30 [13]   R☉
Luminosity57.2±1.2 [13]   L☉
Temperature 5,030±122 [11]   K
Metallicity [Fe/H]−0.16 [12]   dex
Rotational velocity (v sin i)4.1±0.5 [7]  km/s
Bb
Mass 0.58 [8]   M☉
Other designations
10 H. Sextantis, [14] 35 Sex, 68 G. Sextantis [15] , AG+05°1556, BD+05°2384, GC  14745, HD  92841, HIP  52452, HR  4193, SAO  118449, CCDM J10433+0443, TIC  374350811 [16]
Database references
SIMBAD The system
A
B

35 Sextantis (68 G. Sextantis; HD 92841; HR 4193), or simply 35 Sex, is a triple star system located in the equatorial constellation Sextans. The primary has an apparent magnitude of 6.09, [2] making it barely visible to the naked eye, even under ideal conditions. The companion has an apparent magnitude of 7.01, [2] making it readily visible in binoculars, but not to the naked eye. The system is located relatively far at a distance of approximately 700 light-years but it is drifting closer with a combined heliocentric radial velocity of −2.18  km/s . [17]

Contents

The System

A
Separation = 6.8″
Period = 23,000 y
Ba
Separation = 0.021″
Period = 1,580 d
Bb

Hierarchy of orbits in the 35 Sextantis system [9]

The system was first observed by Friedrich Georg Wilhelm von Struve in 1821. [18] The separation between the A and B component was initially 7.90  arcseconds , [18] but it has since decreased to 6.62". [19] Thanks to this separation, the components 35 Sextantis can be distinguished using a telescope. Observations from Tokovinin & Gorynya (2007) revealed that the B component is a single-lined spectroscopic binary. [9] The primary and secondary both take 23,302 years to orbit each other while the secondary and its close companion take 1,568 days to revolve around each other in a relatively eccentric orbit. [9]

Physical characteristic

35 Sextantis A has a stellar classification of K2.5 III, [5] indicating that it is an evolved K-type giant star that has exhausted hydrogen at its core and left the main sequence. 35 Sextantis B has a classification of K1 II-III, [6] indicating that it is a hotter, more evolved K-type star that has the luminosity class intermediate between a bright giant and giant star. The primary has 2.45 times the mass of the Sun [8] but it has expanded to 25.39 times the radius of the Sun. [10] It radiates 240 times the luminosity of the Sun [10] from its enlarged photosphere at an effective temperature of 4,512  K , [11] giving it an orange-hued when viewed in the night sky.

The secondary has a similar mass to the primary [8] but it is smaller, having a radius 10.15 times that of the Sun. [13] 35 Sextantis B radiates 57.2 times the luminosity of the Sun [13] from its photosphere at an effective temperature of 5030 K. [11] Both stars are metal deficient with iron abundances of [Fe/H] = −0.17 and [Fe/H] = −0.16 respectively. [12] They spin modestly with projected rotational velocities of 3.7  km/s and 4.1 km/s. [7] The close companion has a mass 58% that of the Sun's, [8] suggesting that it may be a K-type main-sequence star.

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References

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  15. ↑ Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas". Resultados del Observatorio Nacional Argentino. 1. Bibcode:1879RNAO....1.....G.
  16. ↑ "* 35 Sex". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved January 21, 2024.
  17. ↑ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (January 2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv: astro-ph/0409579 . Bibcode:2005A&A...430..165F. doi: 10.1051/0004-6361:20041272 . S2CID   17804304.
  18. 1 2 Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (December 2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 . ISSN   0004-6256. S2CID   119533755.
  19. ↑ Heintz, W. D. (July 1975). "Micrometer observations of double stars.8". The Astrophysical Journal Supplement Series. 29: 315. Bibcode:1975ApJS...29..315H. doi: 10.1086/190345 . ISSN   0067-0049. S2CID   119454231.
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