“HD 154088”的意思、由来-开放百科全书

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.

Properties

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.^[9] It also has a magnetic cycle similar to the Sun,^[16] though its length is not well constrained.

Planetary system

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.

HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey.^[21] 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.

References

1. ^¹²{{cite journal | title=The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets | last1=Mayor | first1=M. |display-authors=etal | date=2011 | arxiv=1109.2497 |bibcode = 2011arXiv1109.2497M }}
2. ^¹²³⁴⁵⁶{{cite journal | title=Detection of a magnetic field in three old and inactive solar-like planet-hosting stars | last1=Fossati | first1=L. |display-authors=etal | date=2013 | arxiv=1302.0879 | bibcode=2013A&A...551A..85F | doi=10.1051/0004-6361/201220997 | volume=551 | journal=Astronomy | pages=A85}}
3. ^¹{{cite journal | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | last1=Takeda | first1=Genya |display-authors=etal | date=2007 | arxiv=astro-ph/0607235 | bibcode=2007ApJS..168..297T | doi=10.1086/509763 | volume=168 | journal=The Astrophysical Journal Supplement Series | pages=297–318}}
4. ^¹²{{cite journal | title=Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs | last1=Valenti | first1=J. A. | last2=Fischer | first2=D. A. | date=2005 | bibcode=2005ApJS..159..141V | doi=10.1086/430500 | volume=159 | journal=The Astrophysical Journal Supplement Series | pages=141–166}}
5. ^¹²{{cite journal | title=The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities | last1=Lovis | first1=C. |display-authors=etal | date=2011 | arxiv=1107.5325 |bibcode = 2011arXiv1107.5325L }}
6. ^¹{{cite journal | title=The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters | last1=Howard | first1=Andrew A. |display-authors=etal | date=2010 | arxiv=1011.0143 | bibcode=2010Sci...330..653H | doi=10.1126/science.1194854 | volume=330 | journal=Science | pages=653–655 | pmid=21030652}}

词条	HD 154088
释义	Properties Planetary system References {{Starbox begin \| name = HD 154088 }}{{Starbox observe \| epoch = J2000.0 \| constell = Ophiuchus \| ra = {{RA\|17\|04\|27.84}} ± 5.62 \| dec = {{DEC\|-28\|34\|57.64}} ± 3.16 \| appmag_v = 6.7258 ± 0.005 }}{{Starbox character \| class = K0V \| b-v = 0.814 ± 0.034 }}{{Starbox astrometry \| radial_v = 14.2972 ± 0.0003^[5] \| prop_mo_ra = 83.76 ± 0.64 \| prop_mo_dec = -268.69 ± 0.36 \| parallax = 56.06 \| p_error = 0.50 \| parallax_footnote = \| absmag_v = 5.47 ± 0.02 }}{{Starbox detail \| mass = 0.97 ± 0.05^[9] \| metal_fe = 0.31 ± 0.03^[9] \| radius = 0.95 ± 0.03^[11] \| luminosity = 0.68 {{±\|0.06\|0.05}} (log -0.169 ± 0.033)^[12] \| temperature = 5423 ± 51^[9] \| gravity = 4.40 ± 0.11^[9] \| rotational_velocity = 1.9 ± 0.5^[12] \| rotation = 42.6 ± 4.4^[16] \| age_gyr = 3 - 8^[9] }}{{Starbox catalog \| names = {{odlist\|HIP=83541\|GJ=652\|CD=-28° 12769\|SAO=184990}} }}{{Starbox reference \| Simbad = HD+154088 \| EPE = HD+154088 }}{{Starbox end}} 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. Properties 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.^[9] It also has a magnetic cycle similar to the Sun,^[16] though its length is not well constrained. Planetary system 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. {{OrbitboxPlanet begin \| table_ref=^[5] }}{{OrbitboxPlanet \| exoplanet = b \| mass_earth = ≥6.15 ± 0.86 \| period = 18.596 ± 0.021 \| semimajor = 0.1316 ± 0.0021 \| eccentricity = 0.38 ± 0.15 }}{{Orbitbox end}} HD 154088 is also being observed under the Keck Eta-Earth radial velocity survey.^[21] 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. References 1. ^¹²{{cite journal \| title=The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets \| last1=Mayor \| first1=M. \|display-authors=etal \| date=2011 \| arxiv=1109.2497 \|bibcode = 2011arXiv1109.2497M }} 2. ^¹²³⁴⁵⁶{{cite journal \| title=Detection of a magnetic field in three old and inactive solar-like planet-hosting stars \| last1=Fossati \| first1=L. \|display-authors=etal \| date=2013 \| arxiv=1302.0879 \| bibcode=2013A&A...551A..85F \| doi=10.1051/0004-6361/201220997 \| volume=551 \| journal=Astronomy \| pages=A85}} 3. ^¹{{cite journal \| title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog \| last1=Takeda \| first1=Genya \|display-authors=etal \| date=2007 \| arxiv=astro-ph/0607235 \| bibcode=2007ApJS..168..297T \| doi=10.1086/509763 \| volume=168 \| journal=The Astrophysical Journal Supplement Series \| pages=297–318}} 4. ^¹²{{cite journal \| title=Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs \| last1=Valenti \| first1=J. A. \| last2=Fischer \| first2=D. A. \| date=2005 \| bibcode=2005ApJS..159..141V \| doi=10.1086/430500 \| volume=159 \| journal=The Astrophysical Journal Supplement Series \| pages=141–166}} 5. ^¹²{{cite journal \| title=The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities \| last1=Lovis \| first1=C. \|display-authors=etal \| date=2011 \| arxiv=1107.5325 \|bibcode = 2011arXiv1107.5325L }} 6. ^¹{{cite journal \| title=The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters \| last1=Howard \| first1=Andrew A. \|display-authors=etal \| date=2010 \| arxiv=1011.0143 \| bibcode=2010Sci...330..653H \| doi=10.1126/science.1194854 \| volume=330 \| journal=Science \| pages=653–655 \| pmid=21030652}} ^[1]^[2]^[3]^[4]^[5]^[6] }}{{Sky\|17\|04\|27.84\|-\|28\|34\|57.64\|58}}{{Stars of Ophiuchus}} 6 : Ophiuchus (constellation)\|Durchmusterung objects\|Henry Draper Catalogue objects\|Hipparcos objects\|Gliese and GJ objects\|K-type main-sequence stars
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