HO Telescopii: Difference between revisions

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Add: author pars. 1-1. Removed parameters. Some additions/deletions were actually parameter name changes. | You can use this bot yourself. Report bugs here. | Suggested by Abductive | Category:Objects with variable star designations | via #UCB_Category
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{{Starbox begin
{{Starbox begin}}
| name = HO Telescopii
}}
{{Starbox observe
{{Starbox observe
| epoch =
| epoch = J2000.0
| constell = [[Telescopium]]
| equinox =
| ra = {{RA|19|51|58.93159}}<ref name=GaiaDR2/>
| constell = [[Telescopium]]
| ra = {{RA|19|51|58.93064}}<ref name=simbad>{{cite simbad
| dec = {{DEC|−46|51|42.4354}}<ref name=GaiaDR2/>
| appmag_v = 8.22<ref name=Avvakumova_et_al_2013/>&nbsp;(Max)
| title=V* HO Tel
}}
| accessdate=December 16, 2016}}</ref>
{{Starbox character
| dec = {{DEC|-46|51|42.4294}}<ref name=simbad />
| type =
| appmag_v = 8.31<ref name=simbad />
| class = A7III(m)<ref name=houk1978/>
}}
| b-v =
| u-b =
| variable =
}}
{{Starbox astrometry
| radial_v =
| prop_mo_ra = +1.814<ref name=GaiaDR2/>
| prop_mo_dec = −33.369<ref name=GaiaDR2/>
| parallax = 3.5831
| p_error = 0.0796
| parallax_footnote = <ref name=GaiaDR2/>
| absmag_v =
}}
{{Starbox orbit
| reference = <ref name=Sürgit2015/>
| period_unitless = 1.613097&nbsp;d
| axis_unitless = {{val|0.019|0.0001|ul=AU|p=≥}}
| eccentricity = 0.00<ref name=Khaliullin_Khaliullina_2010/>
| inclination = {{val|82.7|0.5}}<ref name=Grygar_Horak_1980/>
| node = <!--Longitude of node (in degrees)-->
| periastron = {{val|2451875.06581|0.00027|ul=HJD|fmt=commas}}
| periarg = <!--Argument of periastron (in degrees), secondary -->
| k1 = {{val|131.11|0.18}}
| k2 = {{val|142.35|0.18}}
}}
{{Starbox detail
| component1 = A
| mass = {{val|1.88|0.04}}<ref name=Sürgit_et_al_2017/>
| radius = {{val|2.28|0.15}}<ref name=Sürgit_et_al_2017/>
| luminosity =
| gravity =
| temperature =
| metal_fe =
| rotation =
| rotational_velocity =
| age_gyr = 1.1<ref name=Sürgit_et_al_2017/>
| component2 = B
| mass2 = {{val|1.73|0.04}}<ref name=Sürgit_et_al_2017/>
| radius2 = {{val|2.08|0.16}}<ref name=Sürgit_et_al_2017/>
}}
{{Starbox catalog
{{Starbox catalog
| names = {{odlist|HD=187418|HIP=97756|SAO=229902|CD=-47° 13121}}<ref name=simbad />
| names = {{odlist | V=HO Tel | HD=187418 | HIP=97756 | SAO=229902 | CD=−47°13121 }}<ref name=SIMBAD/>
}}
{{Starbox reference
| Simbad = HO+Tel
}}
}}
{{Starbox end}}
{{Starbox end}}


'''HO Telescopii''' is an [[eclipsing binary]] [[star]] system located in the southern [[constellation]] of [[Telescopium]]. The maximum [[apparent visual magnitude]] of 8.22<ref name=Avvakumova_et_al_2013/> is too faint to be visible to the naked eye. The system is located at a distance of approximately 910&nbsp;[[light year]]s based on [[stellar parallax|parallax]].<ref name=GaiaDR2/> The combined [[stellar classification]] of the system is A7III(m),<ref name=houk1978/> matching an [[stellar evolution|evolved]] [[A-type star]]<ref name=Spoelstra_Van_Houten_1972/> that is possibly [[Am star|metallic-lined]]. The system is around 1.1<ref name=Sürgit_et_al_2017/>&nbsp;billion years old and consists of two stars of similar mass and size.<ref name=Sürgit_et_al_2017/>
'''HO Telescopii''' is an [[Algol variable]] located in the constellation of [[Telescopium]] that is composed of two [[A-type star|type A stars]], and they have a period of 1.6131409 [[days]].<ref name=a>{{cite journal

| bibcode=1972A&AS....7...83S| title=Five-colour photometry of the eclipsing binary HO Telescopii| journal=Astronomy and Astrophysics Supplement| volume=7| pages=83| last1=Spoelstra| first1=T. A. Th.| last2=Van Houten| first2=C. J.| year=1972}}</ref>
The variability of this system was discovered by W. Strohmeier, R. Knigge, and H. Ott in 1965.<ref name=Sistero_Candellero_1979/><ref name=Strohmeier_et_al_1965/> It is a detached binary system with both components filling three-fourths of their respective [[Roche lobe]]s.<ref name=Sürgit_et_al_2017/> Their [[orbital period]] is {{val|1.613097|fmt=commas}}<ref name=Sürgit2015/>&nbsp;days with a circularized orbit,<ref name=Khaliullin_Khaliullina_2010/> and the [[orbital plane]] is inclined by 83° to the [[Line-of-sight propagation|line of sight]] from the [[Earth]]; close to edge-on.<ref name=Grygar_Horak_1980/> As a consequence, they form an [[Algol variable|Algol-like eclipsing binary]] with a magnitude decrease of 0.51 during the primary eclipse and 0.45 during the secondary eclipse.<ref name=Avvakumova_et_al_2013/>


==References==
==References==
{{reflist}}
{{reflist|refs=


<ref name=GaiaDR2>{{Cite Gaia DR2|6671501451113955072}}</ref>
{{Stars of Telescopium}}


<ref name=SIMBAD>{{cite simbad
[[Category:Telescopium (constellation)]]
| title=HO Tel | access-date=2020-12-12 }}</ref>
[[Category:Algol variables]]

<ref name=houk1978>{{cite journal
| last1=Houk | first1=Nancy
| title=Michigan catalogue of two-dimensional spectral types for the HD stars
| volume=2 | publication-place=Ann Arbor
| publisher=Dept. of Astronomy, University of Michigan
| year=1978 | bibcode=1978mcts.book.....H }}</ref>

<ref name=Khaliullin_Khaliullina_2010>{{cite journal
| title=Synchronization and circularization in early-type binaries on main sequence
| last1=Khaliullin | first1=Kh. F. | last2=Khaliullina | first2=A. I.
| journal=Monthly Notices of the Royal Astronomical Society
| volume=401 | issue=1 | pages=257–274 | date=January 2010
| bibcode=2010MNRAS.401..257K | doi=10.1111/j.1365-2966.2009.15630.x }}</ref>

<ref name=Sistero_Candellero_1979>{{cite journal
| title=HO Telescopii: Light Elements
| last1=Sistero | first1=R. F. | last2=Candellero | first2=B. A.
| journal=Information Bulletin on Variable Stars
| volume=1666 | page=1 | date=August 1979
| bibcode=1979IBVS.1666....1S }}</ref>

<ref name=Strohmeier_et_al_1965>{{cite journal
| title=Bright Southern BV-Stars
| display-authors=1 | last1=Strohmeier | first1=W.
| last2=Knigge | first2=R. | last3=Ott | first3=H.
| journal=Information Bulletin on Variable Stars
| volume=81 | page=1 | date=February 1965
| bibcode=1965IBVS...81....1S }}</ref>

<ref name=Sürgit2015>{{cite journal
| title=First Spectroscopic Solutions of Two Southern Eclipsing Binaries: HO Tel and QY Tel
| display-authors=1 | last1=Sürgit | first1=D.
| last2=Erdem | first2=A. | last3=Engelbrecht | first3=C. A.
| last4=van Heerden | first4=P. | last5=Manick | first5=R.
| work=Living Together: Planets, Host Stars and Binaries, Proceedings of a conference held 8-12 September 2014 in Litomyšl, Czech Republic
| editor1-first=Slavek M. | editor1-last=Rucinski
| editor2-first=Guillermo | editor2-last=Torres
| editor3-first=Miloslav | editor3-last=Zejda
| series=ASP Conference Series | publication-place=San Francisco
| publisher=Astronomical Society of the Pacific
| volume=496 | page=258 | date=July 2015
| bibcode=2015ASPC..496..258S }}</ref>

<ref name=Sürgit_et_al_2017>{{cite journal
| title=Absolute parameters of detached binaries in the southern sky - III: HO Tel
| display-authors=1 | last1=Sürgit | first1=D.
| last2=Erdem | first2=A. | last3=Engelbrecht | first3=C. A.
| last4=van Heerden | first4=H. P. | last5=Manick | first5=R.
| journal=New Astronomy
| volume=54 | pages=109–114 | date=July 2017
| bibcode=2017NewA...54..109S | doi=10.1016/j.newast.2017.01.013 }}</ref>

<ref name=Avvakumova_et_al_2013>{{cite journal
| title=Eclipsing variables: Catalogue and classification
| display-authors=1 | last1=Avvakumova | first1=E. A.
| last2=Malkov | first2=O. Yu. | last3=Kniazev | first3=A. Yu.
| journal=Astronomische Nachrichten
| volume=334 | issue=8 | page=860 | date=October 2013
| bibcode=2013AN....334..860A | doi=10.1002/asna.201311942 }}</ref>

<ref name=Grygar_Horak_1980>{{cite journal
| title=Orbital Elements of the Eclipsing Binaries RW CrA and HO Tel from Multicolour Light Curves
| last1=Grygar | first1=J. | last2=Horak | first2=T. B.
| journal=Bulletin of the Astronomical Institute of Czechoslovakia
| volume=31 | page=297 | date=1980
| bibcode=1980BAICz..31..297G }}</ref>

<ref name=Spoelstra_Van_Houten_1972>{{cite journal
| title=Five-colour photometry of the eclipsing binary HO Telescopii
| last1=Spoelstra | first1=T. A. Th. | last2=Van Houten | first2=C. J.
| journal=Astronomy and Astrophysics Supplement
| volume=7 | pages=83 | year=1972
| bibcode=1972A&AS....7...83S }}</ref>

}}

{{Stars of Telescopium}}
<!-- Properties -->
[[Category:A-type giants]]
[[Category:A-type giants]]
[[Category:Am stars]]
[[Category:Algol variables]]
[[Category:Eclipsing binaries]]
[[Category:Eclipsing binaries]]
<!-- Identifiers -->
[[Category:Objects with variable star designations|Telescopii, HO]]
[[Category:Telescopium (constellation)]]
[[Category:Durchmusterung objects]]
[[Category:Durchmusterung objects]]
[[Category:Henry Draper Catalogue objects|187418]]
[[Category:Henry Draper Catalogue objects|187418]]
[[Category:Hipparcos objects|097756]]
[[Category:Hipparcos objects|097756]]
[[Category:Objects with variable star designations|Telescopii, HO]]


{{main-star-stub}}
{{var-star-stub}}
{{multi-star-stub}}

Revision as of 06:05, 13 December 2020

HO Telescopii
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Telescopium
Right ascension 19h 51m 58.93159s[1]
Declination −46° 51′ 42.4354″[1]
Apparent magnitude (V) 8.22[2] (Max)
Characteristics
Spectral type A7III(m)[3]
Astrometry
Proper motion (μ) RA: +1.814[1] mas/yr
Dec.: −33.369[1] mas/yr
Parallax (π)3.5831 ± 0.0796 mas[1]
Distance910 ± 20 ly
(279 ± 6 pc)
Orbit[4]
Period (P)1.613097 d
Semi-major axis (a)≥0.019±0.0001 AU
Eccentricity (e)0.00[5]
Inclination (i)82.7±0.5[6]°
Periastron epoch (T)2,451,875.06581±0.00027 HJD
Semi-amplitude (K1)
(primary)		131.11±0.18 km/s
Semi-amplitude (K2)
(secondary)		142.35±0.18 km/s
Details
A
Mass1.88±0.04[7] M☉
Radius2.28±0.15[7] R☉
Age1.1[7] Gyr
B
Mass1.73±0.04[7] M☉
Radius2.08±0.16[7] R☉
Other designations
HO Tel, CD−47°13121, HD 187418, HIP 97756, SAO 229902[8]
Database references
SIMBADdata

HO Telescopii is an eclipsing binary star system located in the southern constellation of Telescopium. The maximum apparent visual magnitude of 8.22[2] is too faint to be visible to the naked eye. The system is located at a distance of approximately 910 light years based on parallax.[1] The combined stellar classification of the system is A7III(m),[3] matching an evolved A-type star[9] that is possibly metallic-lined. The system is around 1.1[7] billion years old and consists of two stars of similar mass and size.[7]

The variability of this system was discovered by W. Strohmeier, R. Knigge, and H. Ott in 1965.[10][11] It is a detached binary system with both components filling three-fourths of their respective Roche lobes.[7] Their orbital period is 1.613097[4] days with a circularized orbit,[5] and the orbital plane is inclined by 83° to the line of sight from the Earth; close to edge-on.[6] As a consequence, they form an Algol-like eclipsing binary with a magnitude decrease of 0.51 during the primary eclipse and 0.45 during the secondary eclipse.[2]

References

  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 Avvakumova, E. A.; et al. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten. 334 (8): 860. Bibcode:2013AN....334..860A. doi:10.1002/asna.201311942.
  3. ^ a b Houk, Nancy (1978). "Michigan catalogue of two-dimensional spectral types for the HD stars". 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H. {{cite journal}}: Cite journal requires |journal= (help)
  4. ^ a b Sürgit, D.; et al. (July 2015). Rucinski, Slavek M.; Torres, Guillermo; Zejda, Miloslav (eds.). "First Spectroscopic Solutions of Two Southern Eclipsing Binaries: HO Tel and QY Tel". Living Together: Planets, Host Stars and Binaries, Proceedings of a conference held 8-12 September 2014 in Litomyšl, Czech Republic. ASP Conference Series. 496. San Francisco: Astronomical Society of the Pacific: 258. Bibcode:2015ASPC..496..258S.
  5. ^ a b Khaliullin, Kh. F.; Khaliullina, A. I. (January 2010). "Synchronization and circularization in early-type binaries on main sequence". Monthly Notices of the Royal Astronomical Society. 401 (1): 257–274. Bibcode:2010MNRAS.401..257K. doi:10.1111/j.1365-2966.2009.15630.x.
  6. ^ a b Grygar, J.; Horak, T. B. (1980). "Orbital Elements of the Eclipsing Binaries RW CrA and HO Tel from Multicolour Light Curves". Bulletin of the Astronomical Institute of Czechoslovakia. 31: 297. Bibcode:1980BAICz..31..297G.
  7. ^ a b c d e f g h Sürgit, D.; et al. (July 2017). "Absolute parameters of detached binaries in the southern sky - III: HO Tel". New Astronomy. 54: 109–114. Bibcode:2017NewA...54..109S. doi:10.1016/j.newast.2017.01.013.
  8. ^ "HO Tel". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-12-12.
  9. ^ Spoelstra, T. A. Th.; Van Houten, C. J. (1972). "Five-colour photometry of the eclipsing binary HO Telescopii". Astronomy and Astrophysics Supplement. 7: 83. Bibcode:1972A&AS....7...83S.
  10. ^ Sistero, R. F.; Candellero, B. A. (August 1979). "HO Telescopii: Light Elements". Information Bulletin on Variable Stars. 1666: 1. Bibcode:1979IBVS.1666....1S.
  11. ^ Strohmeier, W.; et al. (February 1965). "Bright Southern BV-Stars". Information Bulletin on Variable Stars. 81: 1. Bibcode:1965IBVS...81....1S.
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