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←Membuat halaman berisi '{{Starbox begin | name=70 Ophiuchi }} {{Starbox observe 2s | epoch = J2000 | equinox = <!--Equinox of coordinates (defaults to epoch)--> | constell = Ophiuchus | c...'
 
k dead-url=yes --> url-status=dead (via JWB)
 
(23 revisi perantara oleh 17 pengguna tidak ditampilkan)
Baris 41: Baris 41:
periastron=301.4 }}
periastron=301.4 }}
{{Starbox detail|
{{Starbox detail|
age=? |
metal= |
metal= |
mass=0.92/0.70 |
mass=0.92/0.70 |
Baris 51: Baris 50:
| volume=259 | issue=2 | pages=543–548
| volume=259 | issue=2 | pages=543–548
| url=http://adsabs.harvard.edu/abs/1992A&A...259..543M
| url=http://adsabs.harvard.edu/abs/1992A&A...259..543M
| accessdate=2007-06-05 }}</ref>/&ndash; |
| accessdate=2007-06-05 }}</ref>/– |
rotation= |
rotation= |
luminosity=0.43/0.08 |
luminosity=0.43/0.08 |
temperature=5,300<ref name="aaa259" />/&ndash; |
temperature=5,300<ref name="aaa259" />/– |
age=0.8&nbsp;&times;&nbsp;10<sup>9</sup><ref name="aaa259" /> }}
age=0.8&nbsp;×&nbsp;10<sup>9</sup><ref name="aaa259" /> }}
{{Starbox catalog |
{{Starbox catalog |
names='''70 Oph'''<br /> V2391 Oph, [[Gliese-Jahreiss catalogue|GJ]] 702, [[Harvard Revised catalogue|HR]] 6752, [[Bonner Durchmusterung|BD]] +02°3482, [[Henry Draper catalogue|HD]] 165341, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 4137.00, [[Luyten Half-Second catalogue|LHS]] 458/9, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 123107, Struve 2272, [[Hipparcos catalogue|HIP]] 88601
names='''70 Oph'''{{br}} V2391 Oph, [[Gliese-Jahreiss catalogue|GJ]] 702, [[Harvard Revised catalogue|HR]] 6752, [[Bonner Durchmusterung|BD]] +02°3482, [[Henry Draper catalogue|HD]] 165341, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 4137.00, [[Luyten Half-Second catalogue|LHS]] 458/9, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 123107, Struve 2272, [[Hipparcos catalogue|HIP]] 88601
2E 4004, IDS 18004+0232 AB, TD1 21598, 70 Oph, 1ES 1802+02.5, IRC +00335, UBV 15379, STF 2272AB, 2EUVE J1805+02.4, JP11 2926, UBV M 22611, ADS 11046 AB, EUVE J1805+02.4, N30 4015, UBV M 22609, ADS 11046, GC 24641, PLX 4137, uvby98 100165341 AB, AG+02 2199, GEN# +1.00165341J, PPM 165145, [B10] 4571, BD+02 3482, GJ 702, ROT 5812, p. WDS J1805.5+0230, CCDM J18055+0230AB, HD 165341, SAO 123107, p. WDS J18054+0232AB, Ci 20 1073, HIC 88601, SBC7 660, CSI+02 3482 1, HIP 88601, SBC9 1022, 2E 1802.9+0230, HR 6752, SKY# 32844<br />
2E 4004, IDS 18004+0232 AB, TD1 21598, 70 Oph, 1ES 1802+02.5, IRC +00335, UBV 15379, STF 2272AB, 2EUVE J1805+02.4, JP11 2926, UBV M 22611, ADS 11046 AB, EUVE J1805+02.4, N30 4015, UBV M 22609, ADS 11046, GC 24641, PLX 4137, uvby98 100165341 AB, AG+02 2199, GEN# +1.00165341J, PPM 165145, [B10] 4571, BD+02 3482, GJ 702, ROT 5812, p. WDS J1805.5+0230, CCDM J18055+0230AB, HD 165341, SAO 123107, p. WDS J18054+0232AB, Ci 20 1073, HIC 88601, SBC7 660, CSI+02 3482 1, HIP 88601, SBC9 1022, 2E 1802.9+0230, HR 6752, SKY# 32844{{br}}
'''70 Oph B'''<br />
'''70 Oph B'''{{br}}
LHS 459, CCDM J18055+0230B, IDS 18004+0232 B, ROT 3570, 70 Oph B, CSI+02 3482 11, LFT 1391, TDSC 46270 B,
LHS 459, CCDM J18055+0230B, IDS 18004+0232 B, ROT 3570, 70 Oph B, CSI+02 3482 11, LFT 1391, TDSC 46270 B,
STF 2272B, 1E 1802.9+0229, LSPM J1805+0229b, TYC 434-5212-1, ADS 11046 B, GCRV 10532, LTT 15338, UBV 15378,
STF 2272B, 1E 1802.9+0229, LSPM J1805+0229b, TYC 434-5212-1, ADS 11046 B, GCRV 10532, LTT 15338, UBV 15378,
ASCC 1153898, GJ 702 B, NLTT 45900 , Zkh 272, BD+02 3482B, HD 165341B, 8pc 196.62B }}
ASCC 1153898, GJ 702 B, NLTT 45900, Zkh 272, BD+02 3482B, HD 165341B, 8pc 196.62B }}
}}
}}
{{Starbox reference
{{Starbox reference
Baris 73: Baris 72:
| title =SIMBAD query result: V* V2391 Oph -- Spectroscopic binary
| title =SIMBAD query result: V* V2391 Oph -- Spectroscopic binary
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| accessdate=2009-06-04 }}</ref>
| accessdate=2009-06-04 }}</ref>


==Bintang ganda==
== Bintang ganda ==
Komponen utamanya merupakan [[bintang katai]] kuning-jingga (''yellow-orange dwarf'') variable<ref name="var1">{{cite web
Komponen utamanya merupakan [[bintang katai]] kuning-jingga (''yellow-orange dwarf'')<ref name="var1">{{cite web
| url=http://www.sai.msu.su/groups/cluster/gcvs/cgi-bin/search.cgi?search=V2391+Oph
| url=http://www.sai.msu.su/groups/cluster/gcvs/cgi-bin/search.cgi?search=V2391+Oph
| work=[[General Catalog of Variable Stars]]
| work=[[General Catalog of Variable Stars]]
Baris 82: Baris 81:
| title=GCVS Query= V2391 Oph
| title=GCVS Query= V2391 Oph
| accessdate=2009-06-04
| accessdate=2009-06-04
}}</ref> of [[spectral type]] K0, and the secondary star is an orange [[main sequence]] dwarf of [[spectral type]] K4.<ref name="SIMBAD2">{{cite web
}}</ref> dengan kelas K0, dan [[bintang katai]] jingga K4 (''type K4 orange main sequence dwarf'') .<ref name="SIMBAD2">{{cite web
| url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gl+702+B
| url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gl+702+B
| title =SIMBAD query result: LHS 459 -- High proper-motion Star
| title =SIMBAD query result: LHS 459 -- High proper-motion Star
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| publisher=[[Centre de Données astronomiques de Strasbourg]]
| accessdate=2009-06-04 }}</ref>
| accessdate=2009-06-04 }}</ref>


==Sejarah pengamatan==
== Sejarah pengamatan ==
Bintang ini dimasukkan pertama ke dalam katalog oleh [[William Herschel]] pada akhir abad ke 18 dalam studinya mengenai [[bintang ganda]]. Herschel membuktikan bahwa [[bintang ganda]] bersifat saling tarik menarik (''gravitationally bound'') dimana kedua komponen bintang tersebut mengorbit mengarah ke tengah massanya. Ini merupakan kontribusi penting bagi [[Hukum Newton]] mengenai gravitasi.
This star system was first cataloged by [[William Herschel]] in the late 18th century in his study of binary stars. Herschel proved that this system as a gravitationally bound [[Binary star]] system where the two stars orbited around a common [[center of mass]]. This was an important contribution to the proof that [[Newton's law of universal gravitation]] applied to objects beyond the [[solar system]]. He commented at the time that there was a possible third ''unseen companion'' affecting the orbit of the two visible stars.<ref name="See" />


== Sistem planet yang diklaim ==
==Claims of a planetary system==
In [[1855]], Capt. [[W. S. Jacob]] of the [[Madras Observatory]] of the [[British East India Company|East India Company]] claimed that the orbit of the binary showed an anomaly, and it was "highly probable" that there was a "planetary body in connection with this system".<ref>{{cite journal |last=Jacob |first=W.S. |year=1855 |title=On Certain Anomalies presented by the Binary Star 70 Ophiuchi |journal=Monthly Notices of the Royal Astronomical Society |volume=15 |pages=228 |url=http://books.google.nl/books?id=pQsAAAAAMAAJ&printsec=frontcover&dq=editions:0B0EaWqbmirpeTa2sds}}</ref> [[Thomas Jefferson Jackson See|T. J. J. See]] made a stronger claim for the existence of a dark companion in this system in [[1899]],<ref name="See">{{cite journal |last=See |first=Thomas Jefferson Jackson |authorlink=Thomas Jefferson Jackson See |year=1896 |title=Researches on the Orbit of F.70 Ophiuchi, and on a Periodic Perturbation in the Motion of the System Arising from the Action of an Unseen Body |journal=The Astronomical Journal |volume=16 |pages=17 |doi=10.1086/102368}}</ref> but [[Forest Ray Moulton]] soon published a paper proving that a three-body system with the specified orbital parameters would be highly unstable.<ref>{{cite journal |url=http://www.shpltd.co.uk/jha.pdf |format=PDF|journal=Journal for the history of astronomy |title=A Career of controversy: the anomaly OF T. J. J. See |last=Sherrill |first=Thomas J. |date=[[1999]] |volume=30 |accessdate=2007-08-27}}</ref> The claims by Jacob and See have both been shown to be erroneous.<ref>{{cite journal |last=Heintz |first=W.D. |year=1988 |month=June |title=The Binary Star 70 Ophiuchi Revisited |journal=Journal of the Royal Astronomical Society of Canada |volume=82 |issue=3 |url=http://adsabs.harvard.edu/abs/1988JRASC..82..140H |accessdate=2007-08-27}}</ref> Jacob's claim was probably one of the first for an [[exoplanet]] based on [[astrometry|astrometric]] evidence.<br />
Pada tahun [[1855]], Capt. [[W. S. Jacob]] dari [[Madras Observatory]] di [[British East India Company|East India Company]] mengklaim bahwa pada orbit di [[bintang ganda]] terlihat keanehan, dan hal ini merupakan "probabilitas tertinggi" bahwa terdapat planet pada sistem tersebut.<ref>{{cite journal |last=Jacob |first=W.S. |year=1855 |title=On Certain Anomalies presented by the Binary Star 70 Ophiuchi |journal=Monthly Notices of the Royal Astronomical Society |volume=15 |pages=228 |url=http://books.google.nl/books?id=pQsAAAAAMAAJ&printsec=frontcover&dq=editions:0B0EaWqbmirpeTa2sds}}</ref> [[Thomas Jefferson Jackson See|T. J. J. See]] memperkuat klaim tersebut bahwa terdapat komponen gelap di [[bintang ganda]] tersebut pada tahun [[1899]],<ref name="See">{{cite journal |last=See |first=Thomas Jefferson Jackson |authorlink=Thomas Jefferson Jackson See |year=1896 |title=Researches on the Orbit of F.70 Ophiuchi, and on a Periodic Perturbation in the Motion of the System Arising from the Action of an Unseen Body |journal=The Astronomical Journal |volume=16 |pages=17 |doi=10.1086/102368}}</ref> [[Forest Ray Moulton]] segera menyampaikan bukti bahwa sistem tersebut sangat tidak stabil.<ref>{{cite journal |url=http://www.shpltd.co.uk/jha.pdf |format=PDF|journal=Journal for the history of astronomy |title=A Career of controversy: the anomaly OF T. J. J. See |last=Sherrill |first=Thomas J. |date=1999 |volume=30 |accessdate=2007-08-27}}</ref> Klain dari Jacob dan See segera menjadi klaim yang tidak terbukti.<ref>{{cite journal |last=Heintz |first=W.D. |year=1988 |month=June |title=The Binary Star 70 Ophiuchi Revisited |journal=Journal of the Royal Astronomical Society of Canada |volume=82 |issue=3 |url=http://adsabs.harvard.edu/abs/1988JRASC..82..140H |accessdate=2007-08-27}}</ref>
A claim of a planetary system was again made by [[Dirk Reuyl]] and [[Erik Holberg]] in 1943. The companion was estimated to have a mass one tenth the mass of the [[Sun]].<ref>{{cite journal
Klaim adanya planet diulang lagi oleh [[Dirk Reuyl]] dan [[Erik Holberg]] pada tahun 1943. Komponen tersebut diperkirakan memiliki massa sepuluh kali [[Matahari]].<ref>{{cite journal
| title= On the Existence of a Third Component in the System 70 Ophiuchi
| title= On the Existence of a Third Component in the System 70 Ophiuchi
| author=Reuyl, Dirk; Holmberg, Erik
| author=Reuyl, Dirk; Holmberg, Erik
Baris 99: Baris 98:
| url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1943ApJ....97...41R&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf
| url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1943ApJ....97...41R&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf
| volume=97 | pages=41-46 | year=1943 | month=January | doi=10.1086/144489
| volume=97 | pages=41-46 | year=1943 | month=January | doi=10.1086/144489
| bibcode=1943ApJ....97...41R}}</ref> This caused quite a sensation at the time but later observations have gradually discredited this claim.<ref>{{cite journal
| bibcode=1943ApJ....97...41R}}</ref> Klaim ini sempat terkenal, namun kemudian diabaikan<ref>{{cite journal
| title=The binary star 70 Ophiuchi revisited
| title=The binary star 70 Ophiuchi revisited
| authors=Heintz, W. D.
| authors=Heintz, W. D.
| journal=[[Royal Astronomical Society of Canada]], Journal (ISSN 0035-872X)
| journal=[[Royal Astronomical Society of Canada]], Journal (ISSN 0035-872X)
| url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1988JRASC..82..140H&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf
| url=http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1988JRASC..82..140H&amp;data_type=PDF_HIGH&amp;whole_paper=YES&amp;type=PRINTER&amp;filetype=.pdf
| volume=82 | month=June | year=1988 | month=June | pages=140-145 | bibcode=1988JRASC..82..140H}}</ref>
| volume=82 | month=June | year=1988 | pages=140-145 | bibcode=1988JRASC..82..140H}}</ref>


== Etimologi ==
=== Refining planetary boundaries ===
Nama lainnya untuk bintang ini adalah:
The negative results of past studies does not completely rule out the possibility of planets. In 2006 a [[McDonald Observatory]] team has set limits to the presence of one or more planets around '''70 Ophiuchi''' with masses between 0.46 and 12.8 [[Jupiter masses]] and average separations spanning between 0.05 and 5.2 [[Astronomical Units]].<ref name=search>{{cite journal| title=Detection Limits from the McDonald Observatory Planet Search Program | date= 7 April 2006| author=Wittenmyer, ''et al.'' | journal=The [[Astronomical Journal]]| volume= 132| issue= 1| pages= 177-188| doi= 10.1086/504942| url=http://www.iop.org/EJ/article/1538-3881/132/1/177/205213.web.pdf?request-id=07bc0d13-46f9-401e-afa4-5f9928b3da46}}</ref>


{| class="wikitable"
==See also==
|-
* [[Barnard's Star]]
! nama lain
* [[List of the nearest stars]]
! asal bahasa
* [[Stars and planetary systems in fiction#70 Ophiuchi|70 Ophiuchi in fiction]]
! arti
|-
|宗人四 / Zōngrénsì||[[China]] ||bintang ketiga pada rasi [[Daftar asterisme di Batasan Pasar di Langit#Petugas Upacara Keagamaan|Petugas Upacara Keagamaan]]<ref name=sb0>salah satu rasi bintang menurut bangsa Cina</ref>
|}


Selain [[rasi]] [[Ophiuchus]], bintang ini juga merupakan anggota dari berbagai rasi, asterisma atau kelompok berikut:
==References==
{| class="wikitable"
|-
! nama rasi / asterisma / kelompok
! asal
! arti
! anggota lainnya
|-
|宗人 / Zōngrén||[[China]] ||[[Daftar asterisme di Batasan Pasar di Langit#Petugas Upacara Keagamaan|Petugas Upacara Keagamaan]]||[[66 Ophiuchi|66 Oph]], [[67 Ophiuchi|66 Oph]], [[68 Ophiuchi|66 Oph]]
|-
|Bull of Poniatowski<ref>{{Cite web |url=http://www.urania.be/showfile.php?id=3095 |title=Salinan arsip |access-date=2011-01-01 |archive-date=2011-01-01 |archive-url=https://web.archive.org/web/20110101152113/http://www.urania.be/showfile.php?id=3095 |url-status=dead }}</ref> || ||banteng Poniatowski||[[67 Ophiuchi|67 Oph]], [[68 Ophiuchi|68 Oph]], [[66 Ophiuchi|66 Oph]], [[73 Ophiuchi|73 Oph]]
|}

== Referensi ==
{{Reflist}}
{{Reflist}}


== Pranala luar ==
==External links==
*[http://arxiv.org/abs/astro-ph/0604171 Detection Limits from the McDonald Observatory Planet Search Program]
* [http://arxiv.org/abs/astro-ph/0604171 Detection Limits from the McDonald Observatory Planet Search Program]
* {{cite web |
* {{cite web |
title=70 Ophiuchi |
title=70 Ophiuchi |
work=SolStation |
work=SolStation |
url=http://www.solstation.com/stars/70ophiu2.htm |
url=http://www.solstation.com/stars/70ophiu2.htm |
accessdate=October 24 2005 |
accessdate=October 24, 2005}}
⚫
<!--{{Sky|18|05|27.3|-|02|30|00|16.64}}-->
dateformat=mdy}}
⚫
{{Sky|18|05|27.3|-|02|30|00|16.64}}

{{Stars of Ophiuchus}}

[[Category:Binary stars]]
[[Category:Flamsteed objects|Ophiuchi, 70]]
[[Category:Ophiuchus constellation]]
[[Category:K-type main sequence stars]]


[[Kategori:Rasi bintang Ophiuchus]]
[[es:70 Ophiuchi]]
[[fr:70 Ophiuchi]]
[[ko:뱀주인자리 70]]
[[it:70 Ophiuchi]]
[[ja:へびつかい座70番星]]
[[ru:70 Змееносца]]
[[sk:70 Ophiuchi]]
[[fi:70 Ophiuchi]]

Revisi terkini sejak 17 September 2021 01.37


}}

70 Ophiuchi
Data pengamatan
Epos J2000      Ekuinoks
Rasi bintang Ophiuchus
'70 Oph'[1]
Asensio rekta  18j 05m 27.285d[1]
Deklinasi  +02° 30′ 00.36″[1]
Magnitudo semu (V) 4.03[1]
'70 Oph B'[2]
Asensio rekta  18j 05m 27.421d[2]
Deklinasi  +02° 29′ 56.42″[2]
Magnitudo semu (V) 6.00[2]
Ciri-ciri
Kelas spektrum K0V[1]/K4V[2]
Magnitudo semu (B) ~4.89[1]/~7.15[2]
Magnitudo semu (V) ~4.03[1]/~6.00[2]
Magnitudo semu (R) -/~5.6[2]
Indeks warna U−B 0.57/?
Indeks warna B−V 0.78/?
Jenis variabel BY[3]/-
Astrometri
Kecepatan radial (Rv)-6.9 km/s
Gerak diri (μ) RA: 124.56 mdb/thn
Dek.: -962.66 mdb/thn
Paralaks (π)195,96±0,87 mdb
Jarak16,64 ± 0,07 tc
(5,10 ± 0,02 pc)
Magnitudo mutlak (MV)5.48/7.51
Orbit bintang ganda visual
Bintang sekunder 70 Oph B
Periode (P) 88.3 tahun
Sumbu semi-mayor (a) 4.56"
Eksentrisitas (e) 0.495
Inklinasi (i) 120.8°
Bujur node (Ω) 13.2°
Epoch periastron (T) 301.4
Detail
Massa0.92/0.70 M☉
Radius0.89/0.73 R☉
Luminositas0.43/0.08 L☉
Gravitasi permukaan (log g)4.5[4]/–
Suhu5,300[4]/– K
Usia0.8 × 109[4] tahun
Penamaan lain
70 Oph
V2391 Oph, GJ 702, HR 6752, BD +02°3482, HD 165341, GCTP 4137.00, LHS 458/9, SAO 123107, Struve 2272, HIP 88601

2E 4004, IDS 18004+0232 AB, TD1 21598, 70 Oph, 1ES 1802+02.5, IRC +00335, UBV 15379, STF 2272AB, 2EUVE J1805+02.4, JP11 2926, UBV M 22611, ADS 11046 AB, EUVE J1805+02.4, N30 4015, UBV M 22609, ADS 11046, GC 24641, PLX 4137, uvby98 100165341 AB, AG+02 2199, GEN# +1.00165341J, PPM 165145, [B10] 4571, BD+02 3482, GJ 702, ROT 5812, p. WDS J1805.5+0230, CCDM J18055+0230AB, HD 165341, SAO 123107, p. WDS J18054+0232AB, Ci 20 1073, HIC 88601, SBC7 660, CSI+02 3482 1, HIP 88601, SBC9 1022, 2E 1802.9+0230, HR 6752, SKY# 32844
70 Oph B
LHS 459, CCDM J18055+0230B, IDS 18004+0232 B, ROT 3570, 70 Oph B, CSI+02 3482 11, LFT 1391, TDSC 46270 B, STF 2272B, 1E 1802.9+0229, LSPM J1805+0229b, TYC 434-5212-1, ADS 11046 B, GCRV 10532, LTT 15338, UBV 15378,

ASCC 1153898, GJ 702 B, NLTT 45900, Zkh 272, BD+02 3482B, HD 165341B, 8pc 196.62B
Referensi basis data
SIMBADdata

70 Ophiuchi adalah komponen utama dari sistem bintang ganda yang berada cukup dekat dengan Bumi, yaitu 16.6 tahun cahaya dari Bumi, berada di rasi Ophiuchus. Dengan magnitudo 4.00, bintang ini merupakan bintang cemerlang yang paling redup yang dapat dilihat dalam cahaya kota.[1]

Bintang ganda

[sunting | sunting sumber]

Komponen utamanya merupakan bintang katai kuning-jingga (yellow-orange dwarf)[3] dengan kelas K0, dan bintang katai jingga K4 (type K4 orange main sequence dwarf) .[2]

Sejarah pengamatan

[sunting | sunting sumber]

Bintang ini dimasukkan pertama ke dalam katalog oleh William Herschel pada akhir abad ke 18 dalam studinya mengenai bintang ganda. Herschel membuktikan bahwa bintang ganda bersifat saling tarik menarik (gravitationally bound) dimana kedua komponen bintang tersebut mengorbit mengarah ke tengah massanya. Ini merupakan kontribusi penting bagi Hukum Newton mengenai gravitasi.

Sistem planet yang diklaim

[sunting | sunting sumber]

Pada tahun 1855, Capt. W. S. Jacob dari Madras Observatory di East India Company mengklaim bahwa pada orbit di bintang ganda terlihat keanehan, dan hal ini merupakan "probabilitas tertinggi" bahwa terdapat planet pada sistem tersebut.[5] T. J. J. See memperkuat klaim tersebut bahwa terdapat komponen gelap di bintang ganda tersebut pada tahun 1899,[6] Forest Ray Moulton segera menyampaikan bukti bahwa sistem tersebut sangat tidak stabil.[7] Klain dari Jacob dan See segera menjadi klaim yang tidak terbukti.[8] Klaim adanya planet diulang lagi oleh Dirk Reuyl dan Erik Holberg pada tahun 1943. Komponen tersebut diperkirakan memiliki massa sepuluh kali Matahari.[9] Klaim ini sempat terkenal, namun kemudian diabaikan[10]

Etimologi

[sunting | sunting sumber]

Nama lainnya untuk bintang ini adalah:

nama lain asal bahasa arti
宗人四 / Zōngrénsì China bintang ketiga pada rasi Petugas Upacara Keagamaan[11]

Selain rasi Ophiuchus, bintang ini juga merupakan anggota dari berbagai rasi, asterisma atau kelompok berikut:

nama rasi / asterisma / kelompok asal arti anggota lainnya
宗人 / Zōngrén China Petugas Upacara Keagamaan 66 Oph, 66 Oph, 66 Oph
Bull of Poniatowski[12] banteng Poniatowski 67 Oph, 68 Oph, 66 Oph, 73 Oph

Referensi

[sunting | sunting sumber]
  1. ^ a b c d e f g h "SIMBAD query result: V* V2391 Oph -- Spectroscopic binary". Centre de Données astronomiques de Strasbourg. Diakses tanggal 2009-06-04. 
  2. ^ a b c d e f g h i "SIMBAD query result: LHS 459 -- High proper-motion Star". Centre de Données astronomiques de Strasbourg. Diakses tanggal 2009-06-04. 
  3. ^ a b "GCVS Query= V2391 Oph". General Catalog of Variable Stars. Sternberg Astronomical Institute, Moscow, Russia. Diakses tanggal 2009-06-04. 
  4. ^ a b c Morell, O.; Kallander, D.; Butcher, H. R (1999). "The age of the Galaxy from thorium in G dwarfs, a re-analysis". Astronomy and Astrophysics. 259 (2): 543–548. Diakses tanggal 2007-06-05. 
  5. ^ Jacob, W.S. (1855). "On Certain Anomalies presented by the Binary Star 70 Ophiuchi". Monthly Notices of the Royal Astronomical Society. 15: 228. 
  6. ^ See, Thomas Jefferson Jackson (1896). "Researches on the Orbit of F.70 Ophiuchi, and on a Periodic Perturbation in the Motion of the System Arising from the Action of an Unseen Body". The Astronomical Journal. 16: 17. doi:10.1086/102368. 
  7. ^ Sherrill, Thomas J. (1999). "A Career of controversy: the anomaly OF T. J. J. See" (PDF). Journal for the history of astronomy. 30. Diakses tanggal 2007-08-27. 
  8. ^ Heintz, W.D. (1988). "The Binary Star 70 Ophiuchi Revisited". Journal of the Royal Astronomical Society of Canada. 82 (3). Diakses tanggal 2007-08-27. 
  9. ^ Reuyl, Dirk; Holmberg, Erik (1943). "On the Existence of a Third Component in the System 70 Ophiuchi" (PDF). The Astrophysical Journal. 97: 41–46. Bibcode:1943ApJ....97...41R. doi:10.1086/144489. 
  10. ^ Heintz, W. D. (1988). "The binary star 70 Ophiuchi revisited" (PDF). Royal Astronomical Society of Canada, Journal (ISSN 0035-872X). 82: 140–145. Bibcode:1988JRASC..82..140H. 
  11. ^ salah satu rasi bintang menurut bangsa Cina
  12. ^ "Salinan arsip". Diarsipkan dari versi asli tanggal 2011-01-01. Diakses tanggal 2011-01-01. 

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