HD 139319
In this article, we will explore the topic of HD 139319 in detail, providing an in-depth analysis ranging from its origins to its relevance today. We will delve into the different aspects surrounding HD 139319, offering a comprehensive vision that allows our readers to deeply understand its importance and implications in different areas. Through research, data and testimonies, we seek to shed light on HD 139319 and its impact on society, culture, economics, politics and other relevant fields. What factors have contributed to the evolution of HD 139319 over time? What are the main challenges you currently face? What are the possible future implications of HD 139319? These are some of the questions that we will address in this article, with the aim of providing a complete and enriching vision of this topic. Join us on this tour of HD 139319 and discover everything there is to know about this fascinating topic!
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | 15h 33m 51.0571s |
| Declination | +63° 54′ 25.6950″ |
| Apparent magnitude (V) | 7.46[2] |
| Characteristics | |
| HD 139319A | |
| Spectral type | A8V+K0III [3] |
| Apparent magnitude (g) | 7.39[4] |
| HD 139319B | |
| Spectral type | F7V |
| Apparent magnitude (g) | 9.65[5] |
| Astrometry | |
| HD 139319A | |
| Proper motion (μ) | RA: 11.44±0.03 mas/yr[4] Dec.: 22.39±0.02 mas/yr[4] |
| Parallax (π) | 6.0571±0.0179 mas[4] |
| Distance | 538 ± 2 ly (165.1 ± 0.5 pc) |
| HD 139319B | |
| Radial velocity (Rv) | 1.6±0.7[5] km/s |
| Proper motion (μ) | RA: 12.09±0.02 mas/yr[5] Dec.: 21.278±0.018 mas/yr[5] |
| Parallax (π) | 6.0345 ± 0.0160 mas[5] |
| Distance | 540 ± 1 ly (165.7 ± 0.4 pc) |
| Orbit[6] | |
| Primary | TW Draconis A |
| Companion | TW Draconis B |
| Period (P) | 2.8068491 d |
| Semi-major axis (a) | 0.057 AU |
| Inclination (i) | 86.8° |
| Semi-amplitude (K1) (primary) | 64.05 km/s |
| Semi-amplitude (K2) (secondary) | 150 km/s |
| Details[7] | |
| TW Draconis A | |
| Mass | 2.16±0.11 M☉ |
| Radius | 2.64±0.04 R☉ |
| Surface gravity (log g) | 3.928±0.026 cgs |
| Temperature | 7815±92 K |
| TW Draconis B | |
| Mass | 0.93±0.05 M☉ |
| Radius | 3.66±0.06 R☉ |
| Surface gravity (log g) | 3.314±0.026 cgs |
| Temperature | 4442±32 K |
| Other designations | |
| BD+64 1077, HIP 76196, 2MASS J15335104+6354257, GSC 04184-00061 | |
| HD 139319A: TW Draconis, TYC 4184-61-1, Gaia DR2 1640708022815757568 | |
| HD 139319B: TYC 4184-61-2, Gaia DR2 1640708022815757824 | |
| Database references | |
| SIMBAD | data |
HD 139319 is a ternary system composed of the binary Algol variable star known as TW Draconis, and a main-sequence companion star at a separation of 3 arcseconds.[6] The system lies in the constellation of Draco about 540 light years away.
System
The primary star is an eclipsing, semi-detached binary, the brighter component of which is a pulsating star of Delta Scuti type. Its pulsation frequency is 17.99 cycles per day.[3] Mass transfer between stars is ongoing in the system[8] with a transfer rate of 6.8×10−7M☉/year. The 2.8 day period of the Algol binary is cyclically variable with a period 116.04 years, possibly due to gravitational influence of the distant companion HD 139319B. Another three stars in the system are suspected.[6]
References
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ "TW Dra". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-12-13.
- ^ a b Kim, S.-L.; Lee, J. W.; Kwon, S.-G.; Youn, J.-H.; Mkrtichian, D. E.; Kim, C. (2003), "Search for A–F Spectral type pulsating components in Algol-type eclipsing binary systems", Astronomy & Astrophysics, 405: 231–236, Bibcode:2003A&A...405..231K, doi:10.1051/0004-6361:20030630
- ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c Liao, Wen-Ping; Qian, Sheng-Bang; Zejda, Miloslav; Zhu, Li-Ying; Li, Lin-Jia (2016), "Lunar-based Ultraviolet Telescope study of the well-known Algol-type binary TW Dra", Research in Astronomy and Astrophysics, 16 (6): 009, Bibcode:2016RAA....16...94L, doi:10.1088/1674-4527/16/6/094, S2CID 124656327
- ^ Bozic, H.; Nemravova, J.; Harmanec, P. (2013), "Standard UBV photometry and improved physical properties of TW Dra", Information Bulletin on Variable Stars, 6086: 1, Bibcode:2013IBVS.6086....1B
- ^ Norton, A. J.; Lohr, M. E.; Smalley, B.; Wheatley, P. J.; West, R. G. (2016), "SuperWASP discovery and SALT confirmation of a semi-detached eclipsing binary that contains aδScuti star", Astronomy & Astrophysics, 587: A54, arXiv:1601.03198, Bibcode:2016A&A...587A..54N, doi:10.1051/0004-6361/201526881, S2CID 10625309
