XO-2

Binary star system in the constellation Lynx From Wikipedia, the free encyclopedia

XO-2 is a binary star system about 490 light-years (150 parsecs) away in the constellation Lynx. It consists of two components, XO-2N and XO-2S, both of which host planetary systems.[10]

Apparentmagnitude(V)11.12±0.03[3]
Apparentmagnitude(V)11.18±0.03[3]
Quick facts Observation data Epoch J2000 Equinox J2000, Apparent magnitude (V) ...
XO-2
Observation data
Epoch J2000      Equinox J2000
Constellation Lynx[1]
XO-2S
Right ascension 07h 48m 07.4814s[2]
Declination +50° 13 03.2554[2]
Apparent magnitude (V) 11.12±0.03[3]
XO-2N
Right ascension 07h 48m 06.4723s[4]
Declination +50° 13 32.9206[4]
Apparent magnitude (V) 11.18±0.03[3]
Characteristics
Spectral type K0V + K0V[3]
Astrometry
XO-2S
Radial velocity (Rv)46.94±0.27[2] km/s
Proper motion (μ) RA: −29.308(15) mas/yr[2]
Dec.: −154.233(13) mas/yr[2]
Parallax (π)6.6721±0.0151 mas[2]
Distance489 ± 1 ly
(149.9 ± 0.3 pc)
Absolute magnitude (MV)5.74[5]
XO-2N
Radial velocity (Rv)47.45±0.44[4] km/s
Proper motion (μ) RA: −29.552(15) mas/yr[4]
Dec.: −154.227(11) mas/yr[4]
Parallax (π)6.6588±0.0158 mas[4]
Distance490 ± 1 ly
(150.2 ± 0.4 pc)
Absolute magnitude (MV)5.74[5]
Details[6]
XO-2S
Mass0.9624±0.0073[7] M
Radius1.011±0.019[7] R
Luminosity0.79±0.14 L
Surface gravity (log g)4.420±0.094 cgs
Temperature5,325±37 K
Metallicity [Fe/H]0.32±0.08 dex
Rotation26.0±0.6 d
Rotational velocity (v sin i)1.5±0.3 km/s
Age7.1+2.5
−2.9
 Gyr
XO-2N
Mass0.96±0.05 M
Radius0.998+0.033
−0.032
 R
Luminosity0.70±0.04 L
Surface gravity (log g)4.43±0.10 cgs
Temperature5,290±18 K
Metallicity [Fe/H]0.37±0.07 dex
Rotation41.6±1.1 d
Rotational velocity (v sin i)1.07±0.09 km/s
Age7.8+1.2
−1.3
 Gyr
Other designations
XO-2S: LSPM J0748+5013S, TYC 3413-210-1, GSC 03413-00210, 2MASS J07480748+5013032[8]
XO-2N: BD+50 1471, LSPM J0748+5013N, TOI-1720, TIC 356473034, TYC 3413-5-1, GSC 03413-00005, 2MASS J07480647+5013328[9]
Database references
SIMBADXO-2S
XO-2N
Exoplanet Archivedata
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Star system

This system is unusual in that the stars are not typically referred to as components A & B, but are designated based on their positions in the sky: XO-2N is the northern star and XO-2S is the southern star.

Both of the stars are slightly cooler than the Sun and are nearly identical to each other. The system has a magnitude of 11 and cannot be seen with the naked eye but is visible through a small telescope. These stars are also notable for their large proper motions.[8][9]

XO-2N and XO-2S have a separation of approximately 4,600 AU.[3]

Planetary systems

Two planets were reported to orbit around XO-2S in 2014 using the radial velocity method. One of them is Jupiter-mass and another has a mass comparable to Saturn.[10] A 2024 study found evidence for a third, super-Jupiter mass planet around XO-2S.[11]

More information Companion (in order from star), Mass ...
The XO-2S planetary system[11]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b ≥0.26±0.01 MJ 0.1347±0.0025 18.220±0.001 0.15±0.02
c ≥1.38±0.05 MJ 0.4737+0.0085
−0.0088
120.059±0.013 0.149±0.006
d ≥3.71+1.2
−0.51
 MJ
5.46+0.85
−0.40
4,696+1,133
−489
0.091+0.028
−0.018
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There is one confirmed exoplanet orbiting XO-2N. XO-2Nb, which is classified as a hot Jupiter, was discovered by the XO Telescope using the transit method around XO-2N in 2007. It was initially the only known planet in the system and was referred to as XO-2b.[3] A long-period variation in the radial velocity of XO-2N was detected in 2015, which could be explained by either a second planet or a stellar activity cycle. The stellar activity explanation is considered more likely,[6] and is further supported by a 2024 study.[11]

More information Companion (in order from star), Mass ...
The XO-2N planetary system[a]
Companion
(in order from star)
Mass Semimajor axis
(AU)
Orbital period
(days)
Eccentricity Inclination Radius
b 0.597±0.021 MJ 0.03668(9) 2.615859719(54) <0.006 87.47±0.37° 1.033±0.023 RJ
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See also

Other systems with multiple planet-hosting stars:

Notes

  1. Mass and eccentricity: Damasso et al. 2015[6]
    Other properties: Wang et al. (2025)[7]

References

Further reading

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