Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Ophiuchus |
Right ascension | 17h 04m 27.84s ± 5.62 [1] |
Declination | −28° 34′ 57.64″ ± 3.16 [1] |
Apparent magnitude (V) | 6.7258 ± 0.005 [1] |
Characteristics | |
Spectral type | K0V |
B−V color index | 0.814 ± 0.034 [1] |
Astrometry | |
Radial velocity (Rv) | 14.2972 ± 0.0003 [2] km/s |
Proper motion (μ) |
RA: 83.76 ± 0.64
[1]
mas/
yr Dec.: -268.69 ± 0.36 [1] mas/ yr |
Parallax (π) | 56.06 ± 0.50 mas [1] |
Distance | 58.2 ± 0.5
ly (17.8 ± 0.2 pc) |
Absolute magnitude (MV) | 5.47 ± 0.02 |
Details | |
Mass | 0.97 ± 0.05 [3] M☉ |
Radius | 0.95 ± 0.03 [4] R☉ |
Luminosity | 0.68 +0.06 −0.05 (log -0.169 ± 0.033) [5] L☉ |
Surface gravity (log g) | 4.40 ± 0.11 [3] cgs |
Temperature | 5423 ± 51 [3] K |
Metallicity [Fe/H] | 0.31 ± 0.03 [3] dex |
Rotation | 42.6 ± 4.4 [6] |
Rotational velocity (v sin i) | 1.9 ± 0.5 [5] km/s |
Age | 3 - 8 [3] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 154088 is a seventh magnitude metal-rich K-type main sequence star that lies approximately 58 light-years away in the constellation of Ophiuchus. The star is orbited by a hot Super-Earth.
HD 154088 is a modestly bright star that lies at the bottom of Ophiuchus, near to the border with Scorpius and near to the plane of the Milky Way. The star was recognised as a high proper motion star during the last century, and early Earth-based parallax measurements such as that of the Gliese Catalogue of Nearby Stars indicated a distance of about 50 light-years.
The star has a spectral type of K0V, indicating that it is a main sequence star that is about 350 degrees cooler than the Sun. On the Hertzsprung-Russell diagram (left), the star lies slightly above the main sequence. This is because the star is very metal-rich; with an Fe/H of 0.3 dex the star has about twice the solar abundance of iron, which makes HD 154088 fall into the somewhat vague group of super metal-rich (SMR) stars. The giant planet occurrence rate of Fe/H = 0.3 stars is on the order of 30%, but HD 154088 is not currently known to host any giant planets.
HD 154088 has a pronounced magnetic field. [3] It also has a magnetic cycle similar to the Sun, [6] though its length is not well constrained.
The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 8 to 119 astronomical units. [7]
A planet orbiting HD 154088 discovered with the HARPS spectrograph was announced in September 2011. With a minimum mass of 6 Earth masses, the companion falls into the regime of Super-Earths.
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥6.15 ± 0.86 M🜨 | 0.1316 ± 0.0021 | 18.596 ± 0.021 | 0.38 ± 0.15 | — | — |
HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey. [8] HD 154088 b is a close match for planet candidate 1 (orbital period = 18.1 days, minimum mass = 6.5 M🜨), so they may be the same detection. The planet existence was finally confirmed in 2021. [9]
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Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Ophiuchus |
Right ascension | 17h 04m 27.84s ± 5.62 [1] |
Declination | −28° 34′ 57.64″ ± 3.16 [1] |
Apparent magnitude (V) | 6.7258 ± 0.005 [1] |
Characteristics | |
Spectral type | K0V |
B−V color index | 0.814 ± 0.034 [1] |
Astrometry | |
Radial velocity (Rv) | 14.2972 ± 0.0003 [2] km/s |
Proper motion (μ) |
RA: 83.76 ± 0.64
[1]
mas/
yr Dec.: -268.69 ± 0.36 [1] mas/ yr |
Parallax (π) | 56.06 ± 0.50 mas [1] |
Distance | 58.2 ± 0.5
ly (17.8 ± 0.2 pc) |
Absolute magnitude (MV) | 5.47 ± 0.02 |
Details | |
Mass | 0.97 ± 0.05 [3] M☉ |
Radius | 0.95 ± 0.03 [4] R☉ |
Luminosity | 0.68 +0.06 −0.05 (log -0.169 ± 0.033) [5] L☉ |
Surface gravity (log g) | 4.40 ± 0.11 [3] cgs |
Temperature | 5423 ± 51 [3] K |
Metallicity [Fe/H] | 0.31 ± 0.03 [3] dex |
Rotation | 42.6 ± 4.4 [6] |
Rotational velocity (v sin i) | 1.9 ± 0.5 [5] km/s |
Age | 3 - 8 [3] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
HD 154088 is a seventh magnitude metal-rich K-type main sequence star that lies approximately 58 light-years away in the constellation of Ophiuchus. The star is orbited by a hot Super-Earth.
HD 154088 is a modestly bright star that lies at the bottom of Ophiuchus, near to the border with Scorpius and near to the plane of the Milky Way. The star was recognised as a high proper motion star during the last century, and early Earth-based parallax measurements such as that of the Gliese Catalogue of Nearby Stars indicated a distance of about 50 light-years.
The star has a spectral type of K0V, indicating that it is a main sequence star that is about 350 degrees cooler than the Sun. On the Hertzsprung-Russell diagram (left), the star lies slightly above the main sequence. This is because the star is very metal-rich; with an Fe/H of 0.3 dex the star has about twice the solar abundance of iron, which makes HD 154088 fall into the somewhat vague group of super metal-rich (SMR) stars. The giant planet occurrence rate of Fe/H = 0.3 stars is on the order of 30%, but HD 154088 is not currently known to host any giant planets.
HD 154088 has a pronounced magnetic field. [3] It also has a magnetic cycle similar to the Sun, [6] though its length is not well constrained.
The survey in 2015 have ruled out the existence of any additional stellar companions at projected distances from 8 to 119 astronomical units. [7]
A planet orbiting HD 154088 discovered with the HARPS spectrograph was announced in September 2011. With a minimum mass of 6 Earth masses, the companion falls into the regime of Super-Earths.
Companion (in order from star) |
Mass |
Semimajor axis ( AU) |
Orbital period ( days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b | ≥6.15 ± 0.86 M🜨 | 0.1316 ± 0.0021 | 18.596 ± 0.021 | 0.38 ± 0.15 | — | — |
HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey. [8] HD 154088 b is a close match for planet candidate 1 (orbital period = 18.1 days, minimum mass = 6.5 M🜨), so they may be the same detection. The planet existence was finally confirmed in 2021. [9]
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cite journal}}
: Cite journal requires |journal=
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help)
{{
cite journal}}
: Cite journal requires |journal=
(
help)