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(Redirected from HD 145457 b)
HD 145457 / Kamuy
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Corona Borealis
Right ascension 16h 10m 03.91440s [1]
Declination +26° 44′ 33.8932″ [1]
Apparent magnitude (V) 6.57 [2]
Characteristics
Evolutionary stage Giant [3]
Spectral type K0 III [4]
B−V color index +1.037±0.005 [2]
Astrometry
Radial velocity (Rv)−3.25±0.12 [1] km/s
Proper motion (μ) RA: −18.354  mas/ yr [1]
Dec.: +36.856  mas/ yr [1]
Parallax (π)7.3867 ± 0.0153  mas [1]
Distance441.5 ± 0.9  ly
(135.4 ± 0.3  pc)
Absolute magnitude (MV)1.09 [2]
Details
Mass1.57±0.46 [3]  M
Radius10.49+0.13
−0.41
[5]  R
Luminosity49.97±0.27 [5]  L
Surface gravity (log g)2.72±0.11 [3]  cgs
Temperature4,738+95
−28
[5]  K
Metallicity [Fe/H]−0.177 [6]  dex
Age5.2 [6]  Gyr
Other designations
BD+27°2595, HD 145457, HIP 79219, SAO 84223 [7]
Database references
SIMBAD data

HD 145457 is a star located in the northern constellation of Corona Borealis (The Northern Crown) at a distance of around 442  light-years from the Sun, [1] as determined through parallax measurements. It has been formally named Kamuy by the IAU, [8] after a spiritual or divine being in Ainu mythology. With an apparent magnitude of 6.57, [9] it is barely visible to the unaided eye on dark nights clear of light pollution. It is drifting closer to the Sun with a radial velocity of −3.2 km/s. [1]

HD 145457 is an aging giant star with a stellar classification of K0 III [4] that has cooled and expanded off the main sequence after exhausting its core hydrogen supply. With the assumption that it is a helium-burning object, the properties of HD 145457 can be derived by comparison with evolutionary tracks. [10] With an age of 5.2 billion years old, [6] it is around 1.57 times as massive as the Sun [3] and has swollen to around 10 times its diameter. It is radiating 50 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,738 K. [5]

It is a lithium-rich giant, unusual since lithium is rapidly destroyed once a star becomes a red giant. One explanation for the excess lithium in these stars has been a recent engulfment of a planet, but it is now thought more likely to be due to nucleosynthesis in the star. It is generally assumed that these lithium-rich giants are members of the red clump, core helium burning stars at the cool end of the horizontal branch. [11]

Planetary system

HD 145457 has an exoplanetary companion called HD 145457 b discovered in 2010. 2.9 times as massive as Jupiter, it orbits about every 176 days with an orbital eccentricity of 0.112±3.1. Its semimajor axis is 0.76 AU. HD 145457 b was discovered by precise Doppler measurements with the Subaru Telescope. [9]

As part of the IAU NameExoWorlds project in 2019, HD 145457 b has been formally named Chura. The name was selected by Japan. Chura is a word in the Ryukyuan/ Okinawan language meaning natural beauty. [8]

The HD 145457 planetary system [12]
Companion
(in order from star)
Mass Semimajor axis
( AU)
Orbital period
( days)
Eccentricity Inclination Radius
b ≥2.794+0.132
−0.117
  MJ
0.762±0.001 176.13+0.18
−0.20
0.111+0.039
−0.040

References

  1. ^ a b c d e f g Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID  244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971. Bibcode: 2012AstL...38..331A. doi: 10.1134/S1063773712050015. S2CID  119257644.
  3. ^ a b c d Feuillet, Diane K.; et al. (2016). "Determining Ages of APOGEE Giants with Known Distances". The Astrophysical Journal. 817 (1): 40. arXiv: 1511.04088. Bibcode: 2016ApJ...817...40F. doi: 10.3847/0004-637X/817/1/40. S2CID  118675933.
  4. ^ a b Heard, John Frederick (1956). "The radial velocities, spectral classes and photographic magnitudes of 1041 late-type stars". Publications of the David Dunlap Observatory. 2 (4). University of Toronto, Toronto, Canada: University of Toronto Press: 107–143. Bibcode: 1956PDDO....2..107H.
  5. ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ a b c Ting, Yuan-Sen; Rix, Hans-Walter (2019). "The Vertical Motion History of Disk Stars throughout the Galaxy". The Astrophysical Journal. 878 (1): 21. arXiv: 1808.03278. Bibcode: 2019ApJ...878...21T. doi: 10.3847/1538-4357/ab1ea5. S2CID  119211560.
  7. ^ "HD 145457". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-02-04.
  8. ^ a b "Japan". NameExoworlds. IAU. Retrieved 2019-12-30.
  9. ^ a b Sato, Bun'ei; et al. (2010). "Substellar Companions to Evolved Intermediate-Mass Stars: HD 145457 and HD 180314". Publications of the Astronomical Society of Japan. 62 (4): 1063–69. arXiv: 1005.2860. Bibcode: 2010PASJ...62.1063S. doi: 10.1093/pasj/62.4.1063. S2CID  119113950.
  10. ^ Kumar, Yerra Bharat; Reddy, Bacham E.; Lambert, David L. (2011). "Origin of Lithium Enrichment in K Giants". The Astrophysical Journal. 730 (1): L12. arXiv: 1102.2299. Bibcode: 2011ApJ...730L..12K. doi: 10.1088/2041-8205/730/1/L12. S2CID  118383042.
  11. ^ Holanda, N.; Drake, N. A.; Pereira, C. B. (2020). "HD 150382: A Lithium-rich Star at the Early-AGB Stage?". The Astronomical Journal. 159 (1): 9. Bibcode: 2020AJ....159....9H. doi: 10.3847/1538-3881/ab5528.
  12. ^ Teng, Huan-Yu; Sato, Bun'ei; et al. (December 2023). "Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars". Publications of the Astronomical Society of Japan. 75 (6): 1030–1071. arXiv: 2308.05343. Bibcode: 2023PASJ...75.1030T. doi: 10.1093/pasj/psad056.
From Wikipedia, the free encyclopedia
(Redirected from HD 145457 b)
HD 145457 / Kamuy
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Corona Borealis
Right ascension 16h 10m 03.91440s [1]
Declination +26° 44′ 33.8932″ [1]
Apparent magnitude (V) 6.57 [2]
Characteristics
Evolutionary stage Giant [3]
Spectral type K0 III [4]
B−V color index +1.037±0.005 [2]
Astrometry
Radial velocity (Rv)−3.25±0.12 [1] km/s
Proper motion (μ) RA: −18.354  mas/ yr [1]
Dec.: +36.856  mas/ yr [1]
Parallax (π)7.3867 ± 0.0153  mas [1]
Distance441.5 ± 0.9  ly
(135.4 ± 0.3  pc)
Absolute magnitude (MV)1.09 [2]
Details
Mass1.57±0.46 [3]  M
Radius10.49+0.13
−0.41
[5]  R
Luminosity49.97±0.27 [5]  L
Surface gravity (log g)2.72±0.11 [3]  cgs
Temperature4,738+95
−28
[5]  K
Metallicity [Fe/H]−0.177 [6]  dex
Age5.2 [6]  Gyr
Other designations
BD+27°2595, HD 145457, HIP 79219, SAO 84223 [7]
Database references
SIMBAD data

HD 145457 is a star located in the northern constellation of Corona Borealis (The Northern Crown) at a distance of around 442  light-years from the Sun, [1] as determined through parallax measurements. It has been formally named Kamuy by the IAU, [8] after a spiritual or divine being in Ainu mythology. With an apparent magnitude of 6.57, [9] it is barely visible to the unaided eye on dark nights clear of light pollution. It is drifting closer to the Sun with a radial velocity of −3.2 km/s. [1]

HD 145457 is an aging giant star with a stellar classification of K0 III [4] that has cooled and expanded off the main sequence after exhausting its core hydrogen supply. With the assumption that it is a helium-burning object, the properties of HD 145457 can be derived by comparison with evolutionary tracks. [10] With an age of 5.2 billion years old, [6] it is around 1.57 times as massive as the Sun [3] and has swollen to around 10 times its diameter. It is radiating 50 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,738 K. [5]

It is a lithium-rich giant, unusual since lithium is rapidly destroyed once a star becomes a red giant. One explanation for the excess lithium in these stars has been a recent engulfment of a planet, but it is now thought more likely to be due to nucleosynthesis in the star. It is generally assumed that these lithium-rich giants are members of the red clump, core helium burning stars at the cool end of the horizontal branch. [11]

Planetary system

HD 145457 has an exoplanetary companion called HD 145457 b discovered in 2010. 2.9 times as massive as Jupiter, it orbits about every 176 days with an orbital eccentricity of 0.112±3.1. Its semimajor axis is 0.76 AU. HD 145457 b was discovered by precise Doppler measurements with the Subaru Telescope. [9]

As part of the IAU NameExoWorlds project in 2019, HD 145457 b has been formally named Chura. The name was selected by Japan. Chura is a word in the Ryukyuan/ Okinawan language meaning natural beauty. [8]

The HD 145457 planetary system [12]
Companion
(in order from star)
Mass Semimajor axis
( AU)
Orbital period
( days)
Eccentricity Inclination Radius
b ≥2.794+0.132
−0.117
  MJ
0.762±0.001 176.13+0.18
−0.20
0.111+0.039
−0.040

References

  1. ^ a b c d e f g Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID  244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv: 1108.4971. Bibcode: 2012AstL...38..331A. doi: 10.1134/S1063773712050015. S2CID  119257644.
  3. ^ a b c d Feuillet, Diane K.; et al. (2016). "Determining Ages of APOGEE Giants with Known Distances". The Astrophysical Journal. 817 (1): 40. arXiv: 1511.04088. Bibcode: 2016ApJ...817...40F. doi: 10.3847/0004-637X/817/1/40. S2CID  118675933.
  4. ^ a b Heard, John Frederick (1956). "The radial velocities, spectral classes and photographic magnitudes of 1041 late-type stars". Publications of the David Dunlap Observatory. 2 (4). University of Toronto, Toronto, Canada: University of Toronto Press: 107–143. Bibcode: 1956PDDO....2..107H.
  5. ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv: 1804.09365. Bibcode: 2018A&A...616A...1G. doi: 10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ a b c Ting, Yuan-Sen; Rix, Hans-Walter (2019). "The Vertical Motion History of Disk Stars throughout the Galaxy". The Astrophysical Journal. 878 (1): 21. arXiv: 1808.03278. Bibcode: 2019ApJ...878...21T. doi: 10.3847/1538-4357/ab1ea5. S2CID  119211560.
  7. ^ "HD 145457". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-02-04.
  8. ^ a b "Japan". NameExoworlds. IAU. Retrieved 2019-12-30.
  9. ^ a b Sato, Bun'ei; et al. (2010). "Substellar Companions to Evolved Intermediate-Mass Stars: HD 145457 and HD 180314". Publications of the Astronomical Society of Japan. 62 (4): 1063–69. arXiv: 1005.2860. Bibcode: 2010PASJ...62.1063S. doi: 10.1093/pasj/62.4.1063. S2CID  119113950.
  10. ^ Kumar, Yerra Bharat; Reddy, Bacham E.; Lambert, David L. (2011). "Origin of Lithium Enrichment in K Giants". The Astrophysical Journal. 730 (1): L12. arXiv: 1102.2299. Bibcode: 2011ApJ...730L..12K. doi: 10.1088/2041-8205/730/1/L12. S2CID  118383042.
  11. ^ Holanda, N.; Drake, N. A.; Pereira, C. B. (2020). "HD 150382: A Lithium-rich Star at the Early-AGB Stage?". The Astronomical Journal. 159 (1): 9. Bibcode: 2020AJ....159....9H. doi: 10.3847/1538-3881/ab5528.
  12. ^ Teng, Huan-Yu; Sato, Bun'ei; et al. (December 2023). "Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars". Publications of the Astronomical Society of Japan. 75 (6): 1030–1071. arXiv: 2308.05343. Bibcode: 2023PASJ...75.1030T. doi: 10.1093/pasj/psad056.

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