AO Serpentis

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AO Serpentis

A visual band light curve for AO Serpentis, plotted from ASAS-SN data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 15h 58m 18.410s[2]
Declination +17° 16′ 10.00″[2]
Apparent magnitude (V) 11.04±0.09[3]
Characteristics
Spectral type A2[4]
B−V color index 0.22[3]
Variable type β Per + δ Sct[5]
Distance
1,450 ± 10 ly
(444 ± 5 pc)
Absolute magnitude (MV)+1.88±0.03
Secondary
Absolute magnitude (MV)+5.17±0.05
Semi-amplitude
(K1)
(primary)		51.6±1.1 km/s
Semi-amplitude (K2)
(secondary)		270.3±3.6 km/s
Details
Rotational velocity (v sin i)
90±18 km/s
Secondary
Mass0.49±0.02 M☉
Radius1.38±0.02 R☉
Luminosity0.93+0.05
−0.04 L☉
Surface gravity (log g)3.85±0.01 cgs
Temperature4,786±11[4] K
TYC 1496-3-1, GSC 01496-00003, 2MASS J15581840+1716101[6]
Database references
SIMBADdata

AO Serpentis is an

light years based on parallax measurements.[2]

This system was discovered by C. Hoffmeister to be an Algol-type eclipsing binary in 1935.[8] The following year, P. Guthnick and R. Prager reported a brightness variation between 10.5 and 12.0.[9] In 2004, S. -L. Kim and associates determined that one of the components of this system is pulsating with a short period.[10]

This is a semi-detached binary star system with the secondary component completely filling its

radius of the Sun. The orbital plane is inclined by an angle of 90° to the line of sight, causing the secondary component to be completely eclipsed once per orbit.[5] The orbital period shows long-term cyclic variations, changing by up to 0.0051 days every 17.32 years. This may be due to magnetic activity cycles or the influence of a third body. The orbital period as a whole is steadily decreasing at the rate of (−5.39±0.03)×10−7 days yr−1 due to loss of mass and angular momentum by the system.[4]

The physical properties of the stellar components can be explained by a mass transfer. At some point in the past, mass flowed from the (at the time) more massive and evolved secondary component. This has left the primary as an A-type main-sequence star while the secondary is less massive but overly large. The hotter primary component is a Delta Scuti variable that is undergoing radial pulsation with a dominant frequency of 21.852 days−1 and a secondary frequency of 23.484 days−1.[5]

References

  1. ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
  2. ^
    doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR
    .
  3. ^
    ISBN 978-0333750889
    .
  4. ^
    S2CID 122306646
    .
  5. ^
    S2CID 222141749
    , 247.
  6. ^ "AO Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-02-19.
  7. S2CID 125853869
    .
  8. doi:10.1002/asna.19352552202
    .
  9. doi:10.1002/asna.19362602202
    .
  10. Bibcode:2004IBVS.5538....1K
    .
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