HR 7703: Difference between revisions

Coordinates: Sky map 20h 11m 11.93827s, −36° 06′ 04.3610″
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{{Short description|Binary star system in the constellation of Sagittarius}}
{{Sky|20|11|11.93827|-|36|06|04.3610|19.61}}
{{Starbox begin
{{Starbox begin
| name = HR 7703
| name = HR 7703
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| prop_mo_ra = +456.99<ref name="vanLeeuwen2007"/>
| prop_mo_ra = +456.99<ref name="vanLeeuwen2007"/>
| prop_mo_dec = –1574.64<ref name="vanLeeuwen2007"/>
| prop_mo_dec = –1574.64<ref name="vanLeeuwen2007"/>
| parallax = 166.25
| parallax = 166.3272
| p_error = 0.27
| p_error = 0.1065
| parallax_footnote = <ref name="vanLeeuwen2007"/>
| parallax_footnote = <ref name="GaiaEDR3">{{Cite Gaia EDR3|6697578465310949376}}</ref>
| absmag_v = 6.53<ref name="AmmlerVonEiff2012"/>
| absmag_v = 6.53<ref name="AmmlerVonEiff2012"/>
}}
}}
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| component2 = HR 7703 B
| component2 = HR 7703 B
| names2 = LHS 487, LFT 1530, LTT 7989
| names2 = LHS 487, LFT 1530, LTT 7989
}}
{{Starbox reference
| Simbad = CCDM+J20112-3605AB|sn=The system
| Simbad2 = TYC+7453-1391-1|sn2=A
| Simbad3 = LHS+487|sn3=B
}}
{{Starbox image
|image={{Location map|100x100|AlternativeMap=Celestial_map_Sgr.svg
|alt=HR 7703 is located in the constellation Sagittarius
|caption=Location of HR 7703 in the constellation [[Sagittarius (constellation)|Sagittarius]]|border=infobox|mark=Red_circle.svg|width=280
|label=HR 7703
|lat=29.4
|long=15.6
|float=center
}}|caption=
}}
}}
{{Starbox end}}
{{Starbox end}}
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Based upon an annual [[parallax]] shift of 0.16625&nbsp;[[arc second]]s as measured by the [[Hipparcos]] satellite, this system is {{Convert|6.015|pc|ly|abbr=off|lk=on|disp=flip}} from [[Earth]]. It is approaching the [[Solar System]] at a [[Space velocity (astronomy)|velocity]] of approximately 129 kilometers per second.<ref name=aaa418_989/> At this rate, it will make its closest approach in 41,100 years when it comes to within {{Convert|2.05|pc|ly|abbr=off|disp=flip}} of the Sun.<ref name="arXiv1003.2160"/>
Based upon an annual [[parallax]] shift of 0.16625&nbsp;[[arc second]]s as measured by the [[Hipparcos]] satellite, this system is {{Convert|6.015|pc|ly|abbr=off|lk=on|disp=flip}} from [[Earth]]. It is approaching the [[Solar System]] at a [[Space velocity (astronomy)|velocity]] of approximately 129 kilometers per second.<ref name=aaa418_989/> At this rate, it will make its closest approach in 41,100 years when it comes to within {{Convert|2.05|pc|ly|abbr=off|disp=flip}} of the Sun.<ref name="arXiv1003.2160"/>


This star system has been examined for an [[infrared excess|excess of radiation]] in the [[Infrared astronomy|infrared]], The presence of an infrared excess can be taken as an indication of a [[debris disk]] orbiting the star. However, no such excess was discovered around HR 7703.<ref name=apj674_2_1086/> [[Radial velocity]] data collected over a period of 12 years was examined for signs of periodicity caused by a planet orbiting at a distance of 3–6&nbsp;[[Astronomical unit|AU]], but none was detected.<ref name="Wittenmyer2011"/>
This star system has been examined for an [[infrared excess|excess of radiation]] in the [[Infrared astronomy|infrared]]. The presence of an infrared excess can be taken as an indication of a [[debris disk]] orbiting the star. However, no such excess was discovered around HR 7703.<ref name=apj674_2_1086/> [[Radial velocity]] data collected over a period of 12 years was examined for signs of periodicity caused by a planet orbiting at a distance of 3–6&nbsp;[[Astronomical unit|AU]], but none was detected.<ref name="Wittenmyer2011"/> A slight linear trend in the radial velocities of the primary is probably due to the companion star.<ref name="Howard2016"/>


==References==
==References==
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| doi=10.1051/0004-6361:20078357
| doi=10.1051/0004-6361:20078357
| arxiv=0708.1752
| arxiv=0708.1752
| s2cid=18759600
| postscript=.
| postscript=.
}}</ref>
}}</ref>
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| date=September 2010
| date=September 2010
| doi=10.1088/0004-637X/720/2/1290 | bibcode=2010ApJ...720.1290G
| doi=10.1088/0004-637X/720/2/1290 | bibcode=2010ApJ...720.1290G
| arxiv=1007.2681 | postscript=. }}</ref>
| arxiv=1007.2681 | s2cid=118565025 | postscript=. }}</ref>


<ref name=aj132_1_161>{{citation
<ref name=aj132_1_161>{{citation
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| journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170
| journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170
| date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G
| date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G
| arxiv=astro-ph/0603770 | postscript=. }}</ref>
| arxiv=astro-ph/0603770 | s2cid=119476992 | postscript=. }}</ref>


<ref name=aaa418_989>{{citation
<ref name=aaa418_989>{{citation
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| date=May 2004 | doi=10.1051/0004-6361:20035959
| date=May 2004 | doi=10.1051/0004-6361:20035959
| bibcode=2004A&A...418..989N | arxiv=astro-ph/0405198
| bibcode=2004A&A...418..989N | arxiv=astro-ph/0405198
| postscript=. }}</ref>
| s2cid=11027621 | postscript=. }}</ref>


<ref name="MH08">{{citation
<ref name="MH08">{{citation
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| pages=1264–1293 | date=November 2008
| pages=1264–1293 | date=November 2008
| doi=10.1086/591785 | bibcode=2008ApJ...687.1264M | arxiv=0807.1686
| doi=10.1086/591785 | bibcode=2008ApJ...687.1264M | arxiv=0807.1686
| s2cid=27151456
| postscript=. }}</ref>
| postscript=. }}</ref>


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| pages=1086–1105 | date=February 2008
| pages=1086–1105 | date=February 2008
| doi=10.1086/525514 | bibcode=2008ApJ...674.1086T
| doi=10.1086/525514 | bibcode=2008ApJ...674.1086T
| arxiv=0710.5498 | postscript=. }}</ref>
| arxiv=0710.5498 | s2cid=54940779 | postscript=. }}</ref>


<ref name="arXiv1003.2160">{{citation
<ref name="arXiv1003.2160">{{citation
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| journal=Astronomy Letters | volume=36 | issue=3 | pages=220–226
| journal=Astronomy Letters | volume=36 | issue=3 | pages=220–226
| doi=10.1134/S1063773710030060 | arxiv=1003.2160
| doi=10.1134/S1063773710030060 | arxiv=1003.2160
| bibcode=2010AstL...36..220B | postscript=. }}</ref>
| bibcode=2010AstL...36..220B | s2cid=118374161 | postscript=. }}</ref>


<ref name="Wittenmyer2011">{{citation
<ref name="Wittenmyer2011">{{citation
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| last7=Bailey | first7=J.
| last7=Bailey | first7=J.
| title=On the Frequency of Jupiter Analogs
| title=On the Frequency of Jupiter Analogs
| volume=727 | issue=2 | page=102
| journal=The Astrophysical Journal | volume=727 | issue=2 | page=102
| date=February 2011 | arxiv=1011.4720
| date=February 2011 | arxiv=1011.4720
| bibcode=2011ApJ...727..102W
| bibcode=2011ApJ...727..102W
| doi=10.1088/0004-637X/727/2/102 | postscript=. }}</ref>
| doi=10.1088/0004-637X/727/2/102 | s2cid=56204861 | postscript=. }}</ref>


<ref name=aaa468_2_721>{{citation
<ref name=aaa468_2_721>{{citation
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| bibcode=2007A&A...468..721B
| bibcode=2007A&A...468..721B
| arxiv=astro-ph/0703754
| arxiv=astro-ph/0703754
| s2cid=18907128
| postscript=. }}</ref>
| postscript=. }}</ref>


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| doi=10.1051/0004-6361:20000451
| doi=10.1051/0004-6361:20000451
| bibcode=2001A&A...367..521P
| bibcode=2001A&A...367..521P
| arxiv=astro-ph/0012289 | postscript=. }}</ref>
| arxiv=astro-ph/0012289 | s2cid=425754 | postscript=. }}</ref>


<ref name="AmmlerVonEiff2012">{{citation
<ref name="AmmlerVonEiff2012">{{citation
| last1=Ammler-von Eiff | first1=M.
| last1=Ammler-von Eiff | first1=Matthias | last2=Reiners | first2=Ansgar
| last2=Reiners | first2=A.
| title=New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?
| title=New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?
| date=June 2012 | arxiv=1204.2459
| journal=Astronomy & Astrophysics | arxiv=1204.2459
| volume=542 | page=A116 | date=June 2012 | postscript=.
| bibcode=2012A&A...542A.116A
| doi=10.1051/0004-6361/201118724 | postscript=. }}</ref>
| doi=10.1051/0004-6361/201118724 | bibcode=2012A&A...542A.116A | s2cid=53666672 }}</ref>


<ref name="APJSS149_2_423">{{citation
<ref name="APJSS149_2_423">{{citation
| first1= M. C. | last1=Turnbull
| first1= Margaret C. | last1=Turnbull |author-link1=Margaret Turnbull
| first2=J. C. | last2=Tarter
| first2=Jill C. | last2=Tarter |author-link2=Jill Tarter
| title=Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars
| title=Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars
| journal=The Astrophysical Journal Supplement Series
| journal=The Astrophysical Journal Supplement Series
| date=December 2003 | volume=149 | issue=2 | pages=423–436
| date=December 2003 | volume=149 | issue=2 | pages=423–436
| doi=10.1086/379320 | bibcode=2003ApJS..149..423T
| doi=10.1086/379320 | bibcode=2003ApJS..149..423T
| postscript=. }}</ref>
| postscript=. | doi-access=free }}</ref>


<ref name="SIMBAD">{{citation
<ref name="SIMBAD">{{cite simbad
| title= LHS 486 -- High proper-motion Star
| title=HD 191408
| access-date=2014-01-10
| work=SIMBAD Astronomical Database
}}</ref>
| publisher=Centre de Données astronomiques de Strasbourg

| url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HR+7703
<ref name="Howard2016">{{cite journal | title=Limits on Planetary Companions from Doppler Surveys of Nearby Stars | last1=Howard | first1=Andrew W. | last2=Fulton | first2=Benjamin J. | journal=Publications of the Astronomical Society of the Pacific | volume=128 | issue=969 | at=114401 | year=2016 | arxiv=1606.03134 | bibcode=2016PASP..128k4401H | doi=10.1088/1538-3873/128/969/114401 | s2cid=118503912 }}</ref>
| accessdate=2014-01-10
| postscript=.
}}</ref>


}}
}}


==External links==
==External links==
*[http://www.astronexus.com/3duniv/anim-pages/pm-pavo.php Indus and Pavo]
*[https://web.archive.org/web/20050311085433/http://www.astronexus.com/3duniv/anim-pages/pm-pavo.php Indus and Pavo]
* {{citation | title=J. Herschel 5173 AB | work=SolStation | url=http://www.solstation.com/stars/hj5173ab.htm | accessdate=November 6, 2005 }}
* {{citation | title=J. Herschel 5173 AB | work=SolStation | url=http://www.solstation.com/stars/hj5173ab.htm | access-date=November 6, 2005 }}

{{Nearest systems|4}}
{{Nearest systems|4}}
{{Stars of Sagittarius}}
{{Stars of Sagittarius}}


{{DEFAULTSORT:HR 7703}}
[[Category:Sagittarius (constellation)]]
[[Category:Sagittarius (constellation)]]
[[Category:Binary stars]]
[[Category:Binary stars]]
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[[Category:M-type main-sequence stars]]
[[Category:M-type main-sequence stars]]
[[Category:Solar-type stars|Gliese, 0783]]
[[Category:Solar-type stars|Gliese, 0783]]
[[Category:Objects within 100 ly of Earth]]
[[Category:Bright Star Catalogue objects|7703]]
[[Category:HR objects|7703]]
[[Category:Durchmusterung objects]]
[[Category:Gould objects|Sagittarii, 279]]
[[Category:Henry Draper Catalogue objects|191408]]
[[Category:Hipparcos objects|099461]]

Latest revision as of 14:43, 20 August 2023

HR 7703
Observation data
Epoch J2000      Equinox J2000
Constellation Sagittarius
Right ascension 20h 11m 11.93827s[1]
Declination –36° 06′ 04.3610″[1]
Apparent magnitude (V) 5.31[2]/11.50[3]
Characteristics
Spectral type K2.5 V[4] + M4 V[5]
U−B color index +0.43[2]
B−V color index +0.85[2]
Astrometry
Radial velocity (Rv)–129.4[6] km/s
Proper motion (μ) RA: +456.99[1] mas/yr
Dec.: –1574.64[1] mas/yr
Parallax (π)166.3272 ± 0.1065 mas[7]
Distance19.61 ± 0.01 ly
(6.012 ± 0.004 pc)
Absolute magnitude (MV)6.53[8]
Details
HR 7703 A
Mass0.65[9] M
Radius0.66[9] R
Luminosity0.26[9] L
Surface gravity (log g)4.48 ± 0.17[9] cgs
Temperature5,075 ± 43[9] K
Metallicity [Fe/H]–0.56 ± 0.04[9] dex
Rotational velocity (v sin i)1.8 ± 0.2[8] km/s
Age7.7[10] Gyr
HR 7703 B
Mass0.24[11] M
Radius0.28[3] R
Other designations
279 G. Sagittarii, Gliese 783, CD –36°13940, GCTP 4782.00, HD 191408, HIP 99461, SAO 211885.[12]
HR 7703 A: LHS 486, LFT 1529, LTT 7988
HR 7703 B: LHS 487, LFT 1530, LTT 7989
Database references
SIMBADThe system
A
B
HR 7703 is located in the constellation Sagittarius
HR 7703 is located in the constellation Sagittarius
HR 7703
Location of HR 7703 in the constellation Sagittarius

HR 7703 (Gliese 783, 279 G. Sagittarii) is a binary star system in the constellation of Sagittarius. The brighter component has an apparent visual magnitude of 5.31,[2] which means it is visible from suburban skies at night. The two stars are separated by an angle of 7.10″, which corresponds to an estimated semimajor axis of 56.30 AU for their orbit.[11]

Based upon an annual parallax shift of 0.16625 arc seconds as measured by the Hipparcos satellite, this system is 19.62 light-years (6.015 parsecs) from Earth. It is approaching the Solar System at a velocity of approximately 129 kilometers per second.[6] At this rate, it will make its closest approach in 41,100 years when it comes to within 6.7 light-years (2.05 parsecs) of the Sun.[13]

This star system has been examined for an excess of radiation in the infrared. The presence of an infrared excess can be taken as an indication of a debris disk orbiting the star. However, no such excess was discovered around HR 7703.[14] Radial velocity data collected over a period of 12 years was examined for signs of periodicity caused by a planet orbiting at a distance of 3–6 AU, but none was detected.[15] A slight linear trend in the radial velocities of the primary is probably due to the companion star.[16]

References[edit]

  1. ^ a b c d van Leeuwen, F. (November 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 Feinstein, A. (1966), "Photoelectric observations of Southern late-type stars", The Information Bulletin for the Southern Hemisphere, 8: 30, Bibcode:1966IBSH....8...30F.
  3. ^ a b Pasinetti-Fracassini, L. E.; et al. (February 2001), "Catalogue of Stellar Diameters (CADARS)", Astronomy and Astrophysics, 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  4. ^ Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  5. ^ Turnbull, Margaret C.; Tarter, Jill C. (December 2003), "Target Selection for SETI. II. Tycho-2 Dwarfs, Old Open Clusters, and the Nearest 100 Stars", The Astrophysical Journal Supplement Series, 149 (2): 423–436, Bibcode:2003ApJS..149..423T, doi:10.1086/379320.
  6. ^ a b Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics, 418 (3): 989–1019, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959, S2CID 11027621.
  7. ^ 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.
  8. ^ a b Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  9. ^ a b c d e f Ghezzi, L.; et al. (September 2010), "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity", The Astrophysical Journal, 720 (2): 1290–1302, arXiv:1007.2681, Bibcode:2010ApJ...720.1290G, doi:10.1088/0004-637X/720/2/1290, S2CID 118565025.
  10. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID 27151456.
  11. ^ a b Bonavita, M.; Desidera, S. (June 2007), "The frequency of planets in multiple systems", Astronomy and Astrophysics, 468 (2): 721–729, arXiv:astro-ph/0703754, Bibcode:2007A&A...468..721B, doi:10.1051/0004-6361:20066671, S2CID 18907128.
  12. ^ "HD 191408". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2014-01-10.
  13. ^ Bobylev, Vadim V. (March 2010), "Searching for Stars Closely Encountering with the Solar System", Astronomy Letters, 36 (3): 220–226, arXiv:1003.2160, Bibcode:2010AstL...36..220B, doi:10.1134/S1063773710030060, S2CID 118374161.
  14. ^ Trilling, D. E.; et al. (February 2008), "Debris Disks around Sun-like Stars", The Astrophysical Journal, 674 (2): 1086–1105, arXiv:0710.5498, Bibcode:2008ApJ...674.1086T, doi:10.1086/525514, S2CID 54940779.
  15. ^ Wittenmyer, Robert A.; et al. (February 2011), "On the Frequency of Jupiter Analogs", The Astrophysical Journal, 727 (2): 102, arXiv:1011.4720, Bibcode:2011ApJ...727..102W, doi:10.1088/0004-637X/727/2/102, S2CID 56204861.
  16. ^ Howard, Andrew W.; Fulton, Benjamin J. (2016). "Limits on Planetary Companions from Doppler Surveys of Nearby Stars". Publications of the Astronomical Society of the Pacific. 128 (969). 114401. arXiv:1606.03134. Bibcode:2016PASP..128k4401H. doi:10.1088/1538-3873/128/969/114401. S2CID 118503912.

External links[edit]