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{{Short description|Star in the constellation Draco}}
{{Starbox begin}}
{{Starbox begin}}
{{Starbox observe
{{Starbox observe
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| temperature = {{val|5,203|46|fmt=commas}}<ref name="apj771_1_40"/>
| temperature = {{val|5,203|46|fmt=commas}}<ref name="apj771_1_40"/>
| metal_fe = {{val|−0.43|0.08}}<ref name="apj652"/>
| metal_fe = {{val|−0.43|0.08}}<ref name="apj652"/>
| rotational_velocity =
| rotational_velocity = 3.4<ref name=Earle2017/>
| gravity = 4.80<ref name="apj131"/>
| gravity = 4.80<ref name="apj131"/>
| age_gyr = 4.27<ref name="apj652"/>
| age_gyr = 4.27<ref name="apj652"/>
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6.43, this star is a challenge to view with the unaided eye but it can be seen clearly with a small [[telescope]]. Based upon [[Stellar parallax|parallax]] measurements, it is located at a distance of around 42 [[light year]]s from the Sun. The star is drifting closer to the Sun with a [[radial velocity]] of −39&nbsp;km/s,<ref name=Anderson2012/> and is predicted to come to within {{convert|8.112|pc|ly|1|adj=ri1|order=flip|abbr=on}} in around 190,400&nbsp;years.<ref name=Bailer-Jones2018/>
6.43, this star is a challenge to view with the unaided eye but it can be seen clearly with a small [[telescope]]. Based upon [[Stellar parallax|parallax]] measurements, it is located at a distance of around 42 [[light year]]s from the Sun. The star is drifting closer to the Sun with a [[radial velocity]] of −39&nbsp;km/s,<ref name=Anderson2012/> and is predicted to come to within {{convert|8.112|pc|ly|1|adj=ri1|order=flip|abbr=on}} in around 190,400&nbsp;years.<ref name=Bailer-Jones2018/>


This is a [[K-type main sequence star]] with a [[spectral classification]] of K0&nbsp;V. It has about 79% of the [[solar radius|Sun's radius]] and 73% of the [[solar mass]].<ref name="apj771_1_40"/> The star is emitting an [[infrared excess|excess of infrared radiation]] at a wavelength of 70&nbsp;μm, suggesting the presence of an orbiting [[debris disk]].<ref name="apj652"/> It has a low [[metallicity]], with only 37% of the Sun's abundance of elements more massive than helium, and has a relatively high [[proper motion]].<ref name="SIMBAD"/>
This is a [[K-type main sequence star]] with a [[spectral classification]] of K0&nbsp;V. It has about 79% of the [[solar radius|Sun's radius]] and 73% of the [[solar mass]].<ref name="apj771_1_40"/> It is an estimated 4.3&nbsp;billion years old and is spinning with a [[projected rotational velocity]] of 3.4&nbsp;km/s.<ref name=Earle2017/> The star is emitting an [[infrared excess|excess of infrared radiation]] at a wavelength of 70&nbsp;μm, suggesting the presence of an orbiting [[debris disk]].<ref name="apj652"/> It has a low [[metallicity]], with only 37% of the Sun's abundance of elements more massive than helium,<ref name="apj652"/> and has a relatively high [[proper motion]].<ref name=GaiaDR2/><ref name="SIMBAD"/>


==References==
==References==
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<ref name="SIMBAD">{{cite simbad | title=LHS 3287 | accessdate=2009-04-14 }}</ref>
<ref name="SIMBAD">{{cite simbad | title=LHS 3287 | accessdate=2009-04-14 }}</ref>

<ref name=Earle2017>{{citation
| title=Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants
| last1=Luck | first1=R. Earle
| journal=The Astronomical Journal
| volume=153 | issue=1 | id=21 | pages=19 | date=January 2017
| bibcode=2017AJ....153...21L | arxiv=1611.02897
| doi=10.3847/1538-3881/153/1/21 | s2cid=119511744 | postscript=. | doi-access=free }}</ref>


<ref name=Bailer-Jones2018>{{citation
<ref name=Bailer-Jones2018>{{citation
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| volume=609 | id=A8 | pages=16 | date=January 2018
| volume=609 | id=A8 | pages=16 | date=January 2018
| arxiv=1708.08595 | bibcode=2018A&A...609A...8B
| arxiv=1708.08595 | bibcode=2018A&A...609A...8B
| doi=10.1051/0004-6361/201731453 }}</ref>
| doi=10.1051/0004-6361/201731453 | s2cid=119462489 }}</ref>


<ref name=Anderson2012>{{citation
<ref name=Anderson2012>{{citation
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| last2=Soubiran | first2=C. | last3=Belik | first3=S. I.
| last2=Soubiran | first2=C. | last3=Belik | first3=S. I.
| title=A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence
| title=A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence
| journal=Astronomy and Astrophysics | volume=427 | date=2004 | pages=933–936
| journal=Astronomy and Astrophysics | volume=427 | date=2004 | issue=3 | pages=933–936
| bibcode=2004A&A...427..933K | arxiv=astro-ph/0409753
| bibcode=2004A&A...427..933K | arxiv=astro-ph/0409753
| doi=10.1051/0004-6361:20041449 }}</ref>
| doi=10.1051/0004-6361:20041449 | s2cid=204935981 }}</ref>


<ref name="aaass129">{{cite journal
<ref name="aaass129">{{cite journal
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| volume=129 | pages=431–433 | date=1998
| volume=129 | pages=431–433 | date=1998
| title=uvbyβ photoelectric photometric catalogue
| title=uvbyβ photoelectric photometric catalogue
| doi=10.1051/aas:1998195 | doi-access=free
| issue=3 | doi=10.1051/aas:1998195 | doi-access=free
| bibcode=1998A&AS..129..431H }}</ref>
| bibcode=1998A&AS..129..431H }}</ref>


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| issue=1 | id=40 | pages=31 | date=July 2013
| issue=1 | id=40 | pages=31 | date=July 2013
| arxiv=1306.2974 | doi=10.1088/0004-637X/771/1/40
| arxiv=1306.2974 | doi=10.1088/0004-637X/771/1/40
| bibcode=2013ApJ...771...40B | postscript=.
| bibcode=2013ApJ...771...40B | s2cid=14911430 | postscript=.
}} See Table 3.</ref>
}} See Table 3.</ref>


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|author1=Luck, R. Earle |author2=Heiter, Ulrike | title=Dwarfs in the Local Region | date=2006
|author1=Luck, R. Earle |author2=Heiter, Ulrike | title=Dwarfs in the Local Region | date=2006
| journal=The Astronomical Journal
| journal=The Astronomical Journal
| volume=131 | pages=3069–3092
| volume=131 |issue=6 | pages=3069–3092
| doi=10.1086/504080
| doi=10.1086/504080
| bibcode=2006AJ....131.3069L
| bibcode=2006AJ....131.3069L
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| journal=The Astrophysical Journal | volume=652 | issue=2
| journal=The Astrophysical Journal | volume=652 | issue=2
| pages=1674–1693 | doi=10.1086/508449
| pages=1674–1693 | doi=10.1086/508449
| date=2006 | bibcode=2006ApJ...652.1674B|arxiv = astro-ph/0611682 }}</ref>
| date=2006 | bibcode=2006ApJ...652.1674B|arxiv = astro-ph/0611682 | s2cid=14207148
}}</ref>


}}
}}
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[[Category:Henry Draper Catalogue objects|158633]]
[[Category:Henry Draper Catalogue objects|158633]]
[[Category:Hipparcos objects|085235]]
[[Category:Hipparcos objects|085235]]
[[Category:HR objects|6518]]
[[Category:Bright Star Catalogue objects|6518]]

Latest revision as of 02:01, 28 November 2023

HD 158633
Observation data
Epoch J2000      Equinox J2000
Constellation Draco
Right ascension 17h 25m 00.09827s[1]
Declination +67° 18′ 24.1501″[1]
Apparent magnitude (V) 6.44[2]
Characteristics
Spectral type K0 V[2]
U−B color index +0.29[3]
B−V color index +0.76[3]
Astrometry
Radial velocity (Rv)−38.71±0.08[2] km/s
Proper motion (μ) RA: −531.958[1] mas/yr
Dec.: +4.734[1] mas/yr
Parallax (π)78.1653 ± 0.51 mas[1]
Distance41.7 ± 0.3 ly
(12.79 ± 0.08 pc)
Absolute magnitude (MV)5.89[4]
Details
Mass0.729[5] M☉
Radius0.7891±0.0144[5] R☉
Luminosity0.4090±0.0040[5] L☉
Surface gravity (log g)4.80[6] cgs
Temperature5,203±46[5] K
Metallicity [Fe/H]−0.43±0.08[7] dex
Rotational velocity (v sin i)3.4[8] km/s
Age4.27[7] Gyr
Other designations
BD+67°1014, GJ 675, HD 158633, HIP 85235, HR 6518, SAO 17474, LHS 287, LTT 15185[9]
Database references
SIMBADdata

HD 158633 is a main sequence star in the northern constellation of Draco. With an apparent visual magnitude of 6.43, this star is a challenge to view with the unaided eye but it can be seen clearly with a small telescope. Based upon parallax measurements, it is located at a distance of around 42 light years from the Sun. The star is drifting closer to the Sun with a radial velocity of −39 km/s,[2] and is predicted to come to within 26.5 ly (8.1 pc) in around 190,400 years.[10]

This is a K-type main sequence star with a spectral classification of K0 V. It has about 79% of the Sun's radius and 73% of the solar mass.[5] It is an estimated 4.3 billion years old and is spinning with a projected rotational velocity of 3.4 km/s.[8] The star is emitting an excess of infrared radiation at a wavelength of 70 μm, suggesting the presence of an orbiting debris disk.[7] It has a low metallicity, with only 37% of the Sun's abundance of elements more massive than helium,[7] and has a relatively high proper motion.[1][9]

References

[edit]
  1. ^ a b c d e f 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.
  2. ^ a b c d 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 Hauck, B.; Mermilliod, M. (1998). "uvbyβ photoelectric photometric catalogue". Astronomy and Astrophysics Supplement Series. 129 (3): 431–433. Bibcode:1998A&AS..129..431H. doi:10.1051/aas:1998195.
  4. ^ Kovtyukh, V. V.; et al. (2004). "A new Böhm-Vitense gap in the temperature range 5560 to 5610 K in the main sequence". Astronomy and Astrophysics. 427 (3): 933–936. arXiv:astro-ph/0409753. Bibcode:2004A&A...427..933K. doi:10.1051/0004-6361:20041449. S2CID 204935981.
  5. ^ a b c d e Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv:1306.2974, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID 14911430, 40. See Table 3.
  6. ^ Luck, R. Earle; Heiter, Ulrike (2006). "Dwarfs in the Local Region". The Astronomical Journal. 131 (6): 3069–3092. Bibcode:2006AJ....131.3069L. doi:10.1086/504080.
  7. ^ a b c d Beichman, C. A.; et al. (2006). "New Debris Disks Around Nearby Main-Sequence Stars: Impact on the Direct Detection of Planets". The Astrophysical Journal. 652 (2): 1674–1693. arXiv:astro-ph/0611682. Bibcode:2006ApJ...652.1674B. doi:10.1086/508449. S2CID 14207148.
  8. ^ a b Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv:1611.02897, Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, S2CID 119511744, 21.
  9. ^ a b "LHS 3287". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-04-14.
  10. ^ Bailer-Jones, C. A. L. (January 2018), "The completeness-corrected rate of stellar encounters with the Sun from the first Gaia data release", Astronomy & Astrophysics, 609: 16, arXiv:1708.08595, Bibcode:2018A&A...609A...8B, doi:10.1051/0004-6361/201731453, S2CID 119462489, A8


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