ADS 7251

_ In today's world, ADS 7251 plays a fundamental role in our society. Its importance covers a wide range of aspects, from the personal sphere to the professional sphere, including the social and cultural sphere. Increasingly, ADS 7251 has become a topic of interest and debate in various circles, as its influence extends to many areas of our lives. In this article, we will thoroughly explore the impact and relevance of ADS 7251, analyzing its different facets and its connection with aspects as diverse as technology, politics, economics, psychology and culture. Through this exploration, we will be able to better understand the importance and influence that ADS 7251 has in our world today.

ADS 7251
ADS 7251 is located in the constellation Ursa Major
ADS 7251 is located in the constellation Ursa Major
ADS 7251
Location of ADS 7251 in the constellation Ursa Major

Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Major
ADS 7251 A
Right ascension 09h 14m 22.7749s[1]
Declination +52° 41′ 11.792″[1]
Apparent magnitude (V) 7.64[2]
ADS 7251 B
Right ascension 09h 14m 24.6828s[3]
Declination +52h 41m 10.902s[3]
Apparent magnitude (V) 7.70[2]
Characteristics
ADS 7251 A (HD 79210)
Spectral type M0V[4]
Apparent magnitude (B) 9.05[2]
Apparent magnitude (G) 6.976[1]
Apparent magnitude (J) 4.89[a][5]
Apparent magnitude (H) 3.987[a][5]
Apparent magnitude (K) 3.99[a][5]
B−V color index +1.41[6]
J−H color index +0.90[b]
J−K color index +0.90[b]
ADS 7251 B (HD 79211)
Spectral type K7V[4]
Apparent magnitude (B) 9.04[2]
Apparent magnitude (G) 7.054[3]
Apparent magnitude (J) 4.779[a][5]
Apparent magnitude (H) 4.043[a][5]
Apparent magnitude (K) 4.14[a][5]
B−V color index +1.42[6]
J−H color index +0.74[b]
J−K color index +0.64[b]
Astrometry
ADS 7251 A (HD 79210)
Radial velocity (Rv)11.245±0.0007[1] km/s
Proper motion (μ) RA: −1,545.787(18)[1] mas/yr
Dec.: −569.053(18)[1] mas/yr
Parallax (π)157.8879±0.0197 mas[1]
Distance20.657 ± 0.003 ly
(6.3336 ± 0.0008 pc)
Absolute magnitude (MV)8.637[7]
ADS 7251 B
Radial velocity (Rv)12.104±0.0008[3] km/s
Proper motion (μ) RA: −1,573.040(18)[3] mas/yr
Dec.: −659.906(19)[3] mas/yr
Parallax (π)157.8825 ± 0.0211 mas[3]
Distance20.658 ± 0.003 ly
(6.3338 ± 0.0008 pc)
Absolute magnitude (MV)8.712[7]
Orbit[8]
Period (P)975 yr
Semi-major axis (a)16.725″
Eccentricity (e)0.28
Details[9]
A
Mass0.69±0.07 M☉
Radius0.58±0.02 R☉
Luminosity0.0789±0.0038 L☉
Surface gravity (log g)4.68±0.07 cgs
Temperature4,024±51 K
Metallicity −0.05±0.16 dex
Rotation16.3+3.5
−1.3 d
Rotational velocity (v sin i)2.9±1.2 km/s
Age1–7 Gyr
B
Mass0.64±0.07 M☉
Radius0.58±0.03 R☉
Luminosity0.0792±0.0031 L☉
Surface gravity (log g)4.68±0.07 cgs
Temperature4,005±51 K
Metallicity −0.03±0.16 dex
Rotation16.61±0.04 d
Rotational velocity (v sin i)2.3±1.5 km/s
Age1–7 Gyr
Other designations
GJ 338, ADS 7251, WDS J09144+5241
A: BD+53°1320, HD 79210, HIP 45343
B: BD+53°1321, HD 79211, HIP 120005
Database references
SIMBADThe system
A
B
Exoplanet Archivedata

ADS 7251 is a binary star system 6.33 parsecs (20.66 light years) from the Sun. The components are near-identical red dwarfs separated by 17″ in 2019.

The two stars share a mildly eccentric orbit with a semimajor axis of 16.725″ and a period of 975 years. Their separation has closed from 21.1″ when they were discovered by F. G. W. Struve in 1821 to 16.9″ in 2019. Struve also documented two much fainter stars about 3′ from the two red dwarfs.[10]

ADS 7251 A is 0.06 magnitudes (six percent) brighter than ADS 7251 B. A catalogue of MK spectral classes lists both stars as secondary standards, with ADS 7251 A being class M0V and ADS 7251 B being class K7V, noted as being unusual in the brighter star having a later spectral type.[4] Other publications have described the stars as being both K7V, both M0V, or the primary being K7V and the secondary M0V.[11][9]

Planetary system

ADS 7251 B, also known as Gliese 338 B or HD 79211, is orbited by one known planet discovered in 2020 by radial velocity. Though described as a super-Earth by its discovery paper, it is closer in mass to Uranus.[9] An independent confirmation of the planet was published in 2022.[12]

The ADS 7251 B (Gliese 338 B) planetary system[12]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥10.6±1.2 M🜨 0.142±0.005 24.422±0.014 0.109+0.100
−0.075 		— —

Notes

  1. ^ a b c d e f 2MASS infrared magnitudes flagged as unreliable or upper limits
  2. ^ a b c d Calculated from 2MASS magnitudes

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 d Huang, Y.; Liu, X. -W.; Yuan, H. -B.; Xiang, M. -S.; Chen, B. -Q.; Zhang, H. -W. (2015). "Empirical metallicity-dependent calibrations of effective temperature against colours for dwarfs and giants based on interferometric data". Monthly Notices of the Royal Astronomical Society. 454 (3): 2863. arXiv:1508.06080. Bibcode:2015MNRAS.454.2863H. doi:10.1093/mnras/stv1991. S2CID 118487917.
  3. ^ 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.
  4. ^ a b c Kirkpatrick, J. D.; et al. (1991). "A standard stellar spectral sequence in the red/near-infrared - Classes K5 to M9". Astrophysical Journal Supplement Series. 77: 417. Bibcode:1991ApJS...77..417K. doi:10.1086/191611.
  5. ^ a b c d e f Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  6. ^ a b Bobylev, V. V.; Goncharov, G. A.; Bajkova, A. T. (2007). "VizieR Online Data Catalog: Orion Spiral Arm CAtalogue (OSACA) (Bobylev+, 2006)". VizieR On-line Data Catalog. Bibcode:2007yCat..90830821B.
  7. ^ a b Houdebine, Éric R.; Mullan, D. J.; Doyle, J. G.; de la Vieuville, Geoffroy; Butler, C. J.; Paletou, F. (2019). "The Mass-Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs". The Astronomical Journal. 158 (2): 56. arXiv:1905.07921. Bibcode:2019AJ....158...56H. doi:10.3847/1538-3881/ab23fe. S2CID 159041104.
  8. ^ Malkov, O. Yu.; et al. (2012). "Dynamical Masses of a Selected Sample of Orbital Binaries". Astronomy & Astrophysics. 546: 5. Bibcode:2012A&A...546A..69M. doi:10.1051/0004-6361/201219774. A69.
  9. ^ a b c González-Álvarez, E.; Osorio, M. R. Zapatero; Caballero, J. A.; Sanz-Forcada, J.; Béjar, V. J. S.; González-Cuesta, L.; Dreizler, S.; Bauer, F. F.; Rodríguez, E.; Tal-Or, L.; Zechmeister, M. (May 2020). "The CARMENES search for exoplanets around M dwarfs. A super-Earth planet orbiting HD 79211 (GJ 338 B)". Astronomy & Astrophysics. 637: A93. arXiv:2003.13052. Bibcode:2020A&A...637A..93G. doi:10.1051/0004-6361/201937050. ISSN 0004-6361.
  10. ^ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  11. ^ Skiff, B. A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014). 1. Bibcode:2014yCat....1.2023S.
  12. ^ a b Ditomasso, Victoria; et al. (2023), "Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N", The Astronomical Journal, 165 (2): 38, arXiv:2210.12211, Bibcode:2023AJ....165...38D, doi:10.3847/1538-3881/ac9ccd, S2CID 253098124