Upsilon Draconis

In this article, we will explore the fascinating world of Upsilon Draconis and its many facets. Upsilon Draconis is a topic that has captured the attention and interest of many people throughout history, being the object of study, debate and reflection in various disciplines. From its origins to the present, Upsilon Draconis has been a relevant topic that has sparked the interest of experts and fans alike. Throughout these pages, we will analyze its impact on society, its evolution over time, and the different perspectives that exist around Upsilon Draconis. This article aims to offer a comprehensive and enriching vision about Upsilon Draconis, generating a space for reflection and learning for all readers interested in this exciting topic.

Upsilon Draconis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Draco
Right ascension 18h 54m 23.85632s[1]
Declination +71° 17′ 49.8906″[1]
Apparent magnitude (V) 4.827[2]
Characteristics
Spectral type K0 III[3]
U−B color index +1.10[4]
B−V color index +1.15[4]
Astrometry
Radial velocity (Rv)−11.1[2] km/s
Proper motion (μ) RA: +49.53[1] mas/yr
Dec.: +42.11[1] mas/yr
Parallax (π)9.48±0.45 mas[1]
Distance340 ± 20 ly
(105 ± 5 pc)
Absolute bolometric
magnitude (Mbol)		−0.70[2]
Orbit[5]
Period (P)258.48 d
Eccentricity (e)0.21
Periastron epoch (T)2441977.5 JD
Argument of periastron (ω)
(secondary)		298°
Semi-amplitude (K1)
(primary)		6.0 km/s
Details
Mass2.05[6] M☉
Radius19[7] R☉
Luminosity170[6] L☉
Surface gravity (log g)2.53[2] cgs
Temperature4,561±61[6] K
Metallicity +0.01[2] dex
Age1.37[6] Gyr
Other designations
υ Dra, 52 Dra, BD+71° 915, HD 176524, HIP 92782, HR 7180, SAO 9283[8]
Database references
SIMBADdata

Upsilon Draconis (υ Dra) is a binary star[5] system in the northern circumpolar constellation of Draco. It is faintly visible to the naked eye with an apparent visual magnitude of 4.83.[2] Based upon an annual parallax shift of 9.48 mas as measured from Earth, it is located around 340 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.02 due to interstellar dust.[9]

In Chinese, 紫微左垣 (Zǐ Wēi Zuǒ Yuán), meaning Left Wall of Purple Forbidden Enclosure, refers to an asterism consisting of υ Draconis, ι Draconis, η Draconis, ζ Draconis, θ Draconis, 73 Draconis, γ Cephei and 23 Cassiopeiae.[10]

This is a single-lined spectroscopic binary star system with an orbital period of 258.48 days and an eccentricity of 0.21.[5] The primary, component A, is an evolved K-type giant star with a stellar classification of K0 III.[3] It is a suspected barium star, which may indicate the orbiting companion, component B, is a white dwarf star.[11]

The measured angular diameter of the primary, after correction for limb darkening, is 1.69±0.02 mas.[12] At the estimated distance of Upsilon Draconis, this yields a physical size of about 19 times the Sun's radius.[7] It is about 1.37 billion years old with an estimated 2.05 times the mass of the Sun.[6] The star is radiating 170 times the solar luminosity from its photosphere at an effective temperature of 4,561 K.[6]

References

  1. ^ a b c d e van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d e f Luck, R. Earle; Heiter, Ulrike (June 2007), "Giants in the Local Region", The Astronomical Journal, 133 (6): 2464–2486, Bibcode:2007AJ....133.2464L, doi:10.1086/513194.
  3. ^ a b Eggen, O. J. (1962), "Space-velocity vectors for 3483 stars with proper motion and radial velocity", Royal Observatory Bulletin, 51: 79, Bibcode:1962RGOB...51...79E.
  4. ^ a b Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  5. ^ a b c Pourbaix, D.; et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424 (2): 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
  6. ^ a b c d e f Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", Astronomical Journal, 150 (3), 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
  7. ^ a b Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1. The radius (R*) is given by:
  8. ^ "ups Dra -- Spectroscopic binary", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-05-30.
  9. ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430: 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
  10. ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  11. ^ Zacs, L.; et al. (April 1997), "An abundance analysis of the single-lined spectroscopic binaries with barium stars-like orbital elements. I. Analysis and results", Astronomy & Astrophysics Supplement Series, 122: 31–42, Bibcode:1997A&AS..122...31Z, doi:10.1051/aas:1997330.
  12. ^ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039.