Astronomy:HD 150248
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scorpius[1] |
| Right ascension | 16h 41m 49.79351s[2] |
| Declination | −45° 22′ 07.5128″[2] |
| Apparent magnitude (V) | 7.02[3] |
| Characteristics | |
| Spectral type | G3V + ?[4] |
| U−B color index | +0.17[3] |
| B−V color index | +0.68[3] |
| Astrometry | |
| Proper motion (μ) | RA: +62.016[2] mas/yr Dec.: −93.481[2] mas/yr |
| Parallax (π) | 35.958 ± 0.0501[2] mas |
| Distance | 90.7 ± 0.1 ly (27.81 ± 0.04 pc) |
| Absolute magnitude (MV) | +4.90[1] |
| Orbit[5] | |
| Period (P) | 3253.26+0.56 −0.55 days |
| Semi-major axis (a) | 4.46+0.12 −0.13 astronomical unit|AU |
| Eccentricity (e) | 0.66872+0.00090 −0.00092 |
| Inclination (i) | 55.97±0.47° |
| Argument of periastron (ω) (secondary) | 356.59±0.13° |
| Semi-amplitude (K1) (primary) | 1.993±0.002 km/s |
| Details | |
| A | |
| Mass | 0.96±0.01[6] M☉ |
| Radius | 1.02±0.02[5] R☉ |
| Luminosity | 1.16+0.13 −0.11[5] L☉ |
| Surface gravity (log g) | 4.37±0.01[6] cgs |
| Temperature | 5,715±3[6] K |
| Metallicity [Fe/H] | −0.091±0.003[6] dex |
| Rotational velocity (v sin i) | 1.43±0.12[7] km/s |
| Age | 8.10+0.24 −0.39[6] Gyr |
| B | |
| Mass | 140±8[5] MJup |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 150248 is a binary star system[5] in the constellation Scorpius, close to the border with Ara. Its primary component is a G-type star, notable for being a near solar twin.[7] HD 150248's photometric color is also very close to that of the Sun; however, it has a lower abundance of metals, and has an apparent visual magnitude of 7.02. At 8.1 billion years old, this star is over three billion years older than the Sun.
To date, no solar twin with an exact match to that of the Sun has been found. However, there are some stars that come very close to being identical, and thus considered solar twins by the astronomical community. An exact solar twin would be a G2V star with a 5772 K temperature, be 4.6 billion years old, with solar metallicity, and a 0.1% solar luminosity variation.[8] Stars with an age of 4.6 billion years, such as the Sun, are at the most stable state. Proper metallicity and size are also very important to low luminosity variation.[9][10][11]
Both components of this system orbit with an period of 3,253.2 days (8.907 years) and have a high eccentricity of 0.66872, putting the stars as close as 1.48 AU in the periastron, and as distant as 7.42 AU in the apoastron. A circumbinary companion would need to orbit at a separation of at least 18.4 AU to have a stable orbit. Meanwhile, for an S-type companion orbiting either A or B, this would be less than 0.446 and 0.186 AU, respectively.[5]
Comparison to the Sun
| Distance (ly) |
Stellar Type |
Temperature (K) |
Metallicity (dex) |
Age (Gyr) |
Notes | |
|---|---|---|---|---|---|---|
| Sun | 0.00 | G2V | 5,778 | +0.00 | 4.6 | [12] |
| HD 150248 [13] | 88 | G3V | 5,715 | −0.091 | 8.10 |
See also
- List of nearest stars
References
- ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 Przybylski, A.; Kennedy, P. M. (1965). "Radial velocities and three-colour photometry of 166 southern stars". Monthly Notices of the Royal Astronomical Society 131: 95–104. doi:10.1093/mnras/131.1.95. Bibcode: 1965MNRAS.131...95P.
- ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal 132 (1): 161–170. doi:10.1086/504637. Bibcode: 2006AJ....132..161G.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Barbato, D.; Ségransan, D.; Udry, S.; Unger, N.; Bouchy, F.; Lovis, C.; Mayor, M.; Pepe, F. et al. (2023-06-01). "The CORALIE survey for southern extrasolar planets - XIX. Brown dwarfs and stellar companions unveiled by radial velocity and astrometry" (in en). Astronomy & Astrophysics 674: A114. doi:10.1051/0004-6361/202345874. ISSN 0004-6361. Bibcode: 2023A&A...674A.114B. HD 150248's database entry at VizieR.
- ↑ 6.0 6.1 6.2 6.3 6.4 Martos, Giulia; Meléndez, Jorge; Rathsam, Anne; Carvalho-Silva, Gabriela (2023-04-21). "Metallicity and age effects on lithium depletion in solar analogues". Monthly Notices of the Royal Astronomical Society 522 (3): 3217–3226. doi:10.1093/mnras/stad1177. ISSN 0035-8711. Bibcode: 2023MNRAS.522.3217M.
- ↑ 7.0 7.1 dos Santos, Leonardo A. et al. (August 2016). "The Solar Twin Planet Search. IV. The Sun as a typical rotator and evidence for a new rotational braking law for Sun-like stars". Astronomy & Astrophysics 592: 8. doi:10.1051/0004-6361/201628558. A156. Bibcode: 2016A&A...592A.156D.
- ↑ NASA Science Editorial Team (Jan 8, 2013). "Solar Variability and Terrestrial Climate". https://science.nasa.gov/science-news/science-at-nasa/2013/08jan_sunclimate/.
- ↑ "Stellar Luminosity Calculator". http://astro.unl.edu/classaction/animations/stellarprops/stellarlum.html.
- ↑ The Effects of Solar Variability on Earth's Climate. 2012. doi:10.17226/13519. ISBN 978-0-309-26564-5.
- ↑ Ethan Siegel (June 5, 2013). "Most of Earth’s twins aren’t identical". http://scienceblogs.com/startswithabang/2013/06/05/most-of-earths-twins-arent-identical-or-even-close/.
- ↑ Williams, D.R. (2004). "Sun Fact Sheet". NASA. http://nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html.
- ↑ HD 150248 at SIMBAD - Ids - Bibliography - Image.
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