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 | |
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]
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 | |
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]