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V1054 Ophiuchi

{{Short description|Star system in the constellation Ophiuchus}}

{{Sky|16|55|32.0|-|08|21|30|21.05}}

{{Starbox begin

| name = V1054 Ophiuchi

}}

{{Starbox image

| image = 250px

| caption = An ultraviolet band light curve for a flare on V1054 Ophiuchi, plotted from data published by Dal and Evren (2010)

}}

{{Starbox observe 3s

| epoch = J2000.0

| constell = Ophiuchus

| component1 = AB

| ra1 = {{RA|16|55|28.75757}}

| dec1 = {{DEC|-08|20|10.7878}}

| appmag_v1 = 9.74/10.34/10.84

| component2 = Gliese 643

| ra2 = {{RA|16|55|25.22225}}

| dec2 = {{DEC|-08|19|21.2970}}

| appmag_v2 = 11.74

| component3 = C (VB 8)

| ra3 = {{RA|16|55|35.25574}}

| dec3 = {{DEC|-08|23|40.7531}}

| appmag_v3 = 16.80

}}

{{Starbox character

| component1 = AB

| class = M3 V / M4 VeReferred to entire V1054 Ophiuchi Bab subsystem.

}}

{{Starbox character|no_heading=y

| component1 = Gliese 643

| class = M3.5 V

}}

{{Starbox character|no_heading=y

| component1 = C (VB 8)

| class = M7.0 V

}}

{{Starbox astrometry

| component1 = AB

| radial_v = {{val|14.89|0.05}}

| prop_mo_ra = {{val|-817.84|6.68}}

| prop_mo_dec = {{val|-873.53|3.53}}

| pm_footnote =

| parallax = 161.41

| p_error = 5.64

| parallax_footnote =

| absmag_v = 10.23

}}

{{Starbox astrometry|no_heading=y

| component1 = Gliese 643

| radial_v = {{val|15.20|0.15}}

| prop_mo_ra = {{val|-817.580|(52)}}

| prop_mo_dec = {{val|-898.595|(40)}}

| pm_footnote =

| parallax = 153.8754

| p_error = 0.0474

| parallax_footnote =

| absmag_v = 12.60

| component2 = VB 8

| radial_v2 =

| prop_mo_ra2 = {{val|-813.038|(63)}}

| prop_mo_dec2 = {{val|-870.609|(44)}}

| pm_footnote2 =

| parallax2 = 153.9659

| p_error2 = 0.0570

| parallax_footnote2 =

| absmag_v2 = 17.75

}}

{{Starbox orbit

| reference =

| primary = V1054 Oph A

| name = V1054 Oph B

| period = {{val|1.717267|0.000039}}

| axis = {{val|0.2273|0.0004}}

| axis_unitless = {{val|1.46683|ul=AU}}Assuming weighted mean parallax 154.96 mas.

| eccentricity = {{val|0.042|0.001}}

| inclination = {{val|160.3|0.1}}

| node = {{val|-10.2|0.2}}

| periastron = MJD {{val|53943|3}}

| periarg = {{val|306.0|1.5}}

}}

{{Starbox orbit

| reference =

| primary = V1054 Oph Ba

| name = V1054 Oph Bb

| period_unitless = {{val|2.965509|0.000006|ul=d}}

| axis = 0.00687From masses, period and parallax.

| axis_unitless = {{val|0.04432|ul=AU}}From masses and period. According to Mazeh et al. 2001, of order of 0.05 a. u.

| eccentricity = {{val|0.0209|0.0008}}

| inclination = {{val|164.18|0.08}}

| node =

| periastron = MJD {{val|50919.48|0.03}}

| periarg = {{val|150.0|3.0}}

}}

{{Starbox detail

| source =

| component1 = AB

| mass = {{val|0.4155|0.0057}} / {{val|0.3466|0.0047}} / {{val|0.3143|0.0040}}

| component2 = Gliese 643

| mass2 = 0.19

}}

{{Starbox detail|no_heading=y

| reference =

| component1 = C (VB 8)

| mass = {{val|0.0914|0.0026|0.0025}}

| radius = {{val|0.1214|0.0060|0.0057}}

| luminosity = 0.000645{{±|0.000004|0.000005}}

| rotation = {{val|11.19|0.02}} days

| temperature = {{val|2640|65|64|fmt=commas}}

}}

{{Starbox catalog

| names = {{odlist | CCDM=J16555-0820}}

| component1 = AB

| names1 = {{odlist | V=V1054 Oph | BD=−08°4352 | GJ=644 | HD=152751 | HIP=82817 | LHS=428 | SAO=141439 | Wolf=630 }}

| component2 = GJ 643

| names2 = {{odlist | GJ=643 | HIP=82809 | LHS=427 | Wolf=629}}

| component3 = C

| names3 = {{odlist | GJ=644 C | LHS=429}}, VB 8

}}

{{Starbox reference

|Simbad=V*+V1054+Oph|sn=ABab

|Simbad2=Wolf+629|sn2=GJ 643

|Simbad3=GJ+644+C|sn3=C (vB 8)

}}

{{Starbox end}}

V1054 Ophiuchi, together with the star Gliese 643, is a nearby quintuple star system, located in the constellation Ophiuchus at a distance of 21.2 light-years. It consists of five stars, all of which are red dwarfs. The alternative designation of Wolf 630 forms the namesake of a moving group of stars that share a similar motion through space.{{cite journal

| title=Spectroscopic Abundances and Membership in the Wolf 630 Moving Group

| last1=Bubar | first1=Eric J. | last2=King | first2=Jeremy R.

| journal=The Astronomical Journal | volume=140 | issue=2 | pages=293–318 | date=August 2010

| doi=10.1088/0004-6256/140/2/293 | bibcode=2010AJ....140..293B

| arxiv=1005.1205 | s2cid=118455341 }}

Overview

{{tree chart/start}}

{{tree chart|border=1| | | |, |S1| | |S1=A }}

{{tree chart|border=0| | |, |( |PA| | |PA=P = 1.72 yr }}

{{tree chart|border=1| | |! |! |, |S2| |S2=Ba }}

{{tree chart|border=0| | |! |` |( |PB| |PB=P = 2.97 d }}

{{tree chart|border=1| | |! | |` |S3| |S3=Bb }}

{{tree chart|border=0| |,|( |PC| | | |PC=72″ separation }}

{{tree chart|border=1| |!|` |S4| | | |S4=GJ 643 }}

{{tree chart|border=0| |(| |PD| | | |PD=220″ separation }}

{{tree chart|border=1| |`|- |S5| | | |S5=C (VB 8) }}

{{tree chart/end}}

Hierarchy of orbits in the system

V1054 Ophiuchi/Gliese 643 is the nearest quintuple star system; the next nearest star systems with at least five stars are Xi Ursae Majoris (quintuple, including a brown dwarf) at 28.5 light-years, Castor (sextuple) at 49.2 light-years, and GJ 2069 (quintuple) at 54.3 light-years. V1054 Ophiuchi and Xi Ursae Majoris are the only two quintuple star systems within 10 parsecs.

The system consists of three widely separated parts:

  • close triple subsystem V1054 Ophiuchi A-Bab (including very close binary subsystem V1054 Ophiuchi Bab)
  • Gliese 643
  • V1054 Ophiuchi C (vB 8)

The brightest and most massive of these five stars is V1054 Ophiuchi A. The close binary subsystem V1054 Ophiuchi B is more massive than V1054 Ophiuchi A, however, its total visual magnitude is 0.1 mag fainter than V1054 Ophiuchi A's visual magnitude.

The total apparent magnitude of the V1054 Ophiuchi A-Bab triple subsystem is 9.02.

Despite V1054 Ophiuchi/Gliese 643 consisting of low-mass stars, the system's total mass, due to the large number of components, exceeds the Solar mass, (it is about {{Solar mass|1.35|link=y}}).

Distance

Currently, the most accurate distance estimate of V1054 Ophiuchi/Gliese 643 is a trigonometric parallax of Gliese 643 from Gaia DR3: {{val|153.8754|0.0474}} mas, corresponding to a distance of {{val|6.499|0.002}} pc, or {{val|21.196|0.007}} ly.

Past V1054 Ophiuchi/Gliese 643 distance estimates

V1054 Ophiuchi A-Bab:

class="wikitable"
SourcePaperParallax, masDistance, pcDistance, lyRef.
Woolley[http://adsabs.harvard.edu/abs/1970ROAn....5.....W Woolley et al. 1970]156 ± 46.41 ± 0.1720.9 ± 0.6[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=V/32A Vizier, Stars within 25 pc of the Sun (Woolley+ 1970)]
GJ, 3rd version[http://adsabs.harvard.edu/abs/1995yCat.5070....0G Gliese & Jahreiß 1991]153.9 ± 2.66.50 ± 0.1121.19 ± 0.36[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=V/70A Vizier, Nearby Stars, Preliminary 3rd Version (Gliese+ 1991)]
YPC, 4th edition[http://adsabs.harvard.edu/abs/1995GCTP..C......0V van Altena et al. 1995]154.8 ± 0.66.460 ± 0.02521.07 ± 0.08
Hipparcos[http://adsabs.harvard.edu/abs/1997HIP...C......0E Perryman 1997]174.23 ± 3.905.74 ± 0.1318.7 ± 0.4[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=I/239 Vizier, The Hipparcos and Tycho Catalogues (ESA 1997)]
Soederhjelm[http://adsabs.harvard.edu/abs/1999A&A...341..121S Soederhjelm 1999]155.63 ± 1.816.43 ± 0.0820.96 ± 0.25[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=J/A+A/341/121 Vizier, Visual binary orbits and masses (Soederhjelm 1999)]
Hipparcos2[http://adsabs.harvard.edu/abs/2007A&A...474..653V van Leeuwen 2007]161.41 ± 5.646.20 ± 0.2220.21 ± 0.73[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=I/311 Vizier, Hipparcos, the New Reduction (van Leeuwen 2007)]

Gliese 643:

class="wikitable"
SourcePaperParallax, masDistance, pcDistance, lyRef.
Woolley[http://adsabs.harvard.edu/abs/1970ROAn....5.....W Woolley et al. 1970]169 ± 55.92 ± 0.1819.3 ± 0.6
GJ, 3rd version[http://adsabs.harvard.edu/abs/1995yCat.5070....0G Gliese & Jahreiß 1991]171.9 ± 7.35.82 ± 0.2619.0 ± 0.8
YPC, 4th edition[http://adsabs.harvard.edu/abs/1995GCTP..C......0V van Altena et al. 1995]169.8 ± 6.65.89 ± 0.2419.2 ± 0.8
Hipparcos[http://adsabs.harvard.edu/abs/1997HIP...C......0E Perryman 1997]153.96 ± 4.046.50 ± 0.1821.2 ± 0.6
Hipparcos2[http://adsabs.harvard.edu/abs/2007A&A...474..653V van Leeuwen 2007]148.92 ± 4.006.72 ± 0.1921.9 ± 0.6

V1054 Ophiuchi C (vB 8):

class="wikitable"
SourcePaperParallax, masDistance, pcDistance, lyRef.
CTIOPI 1.5 mTSN 14 ([http://adsabs.harvard.edu/abs/2005AJ....130..337C Costa et al. 2005])155.43 ± 1.336.43 ± 0.0620.98 ± 0.18

{{cite journal

| last=Costa |first=Edgardo

|author2=Méndez, René A. |author3=Jao, W.-C. |author4=Henry, Todd J. |author5=Subasavage, John P. |author6=Brown, Misty A. |author7=Ianna, Philip A. |author8= Bartlett, Jennifer |author8-link=Jennifer Bartlett (astronomer)

| year=2005

| title=The Solar Neighborhood. XIV. Parallaxes from the Cerro Tololo Inter-American Observatory Parallax Investigation-First Results from the 1.5 m Telescope Program

| journal=The Astronomical Journal

| volume=130 |issue=1

| pages=337–349

| bibcode=2005AJ....130..337C

| doi=10.1086/430473

|citeseerx=10.1.1.573.7563|s2cid=12213270

}}

=Weighted mean distance=

A weighted mean parallax[http://www.denseproject.com/25pc/ DENSE Project. 25 pc White Dwarf Sample] (see formulae below) was calculated by RECONS in 2012, considering YPC (V1054 Ophiuchi A-Bab and Gliese 643), Hipparcos (Soederhjelm — V1054 Ophiuchi A-Bab and van Leeuwen — Gliese 643) and CTIOPI (V1054 Ophiuchi C) data. The value is {{val|154.96|0.52}} mas,[http://recons.org/TOP100.posted.htm THE ONE HUNDRED NEAREST STAR SYSTEMS brought to you by RECONS (Research Consortium On Nearby Stars)] corresponding to a distance of {{val|6.453|0.022}} pc, or {{val|21.05|0.07}} ly. This predates Gaia astrometry of the system.

System

=V1054 Ophiuchi A-Bab (inner triple subsystem)=

V1054 Ophiuchi A-Bab is a close spectroscopic triple subsystem, consisting of the brighter component V1054 Ophiuchi A and the more massive binary subsystem V1054 Ophiuchi Bab, orbiting each other with a period of 627 days, or 1.72 years. V1054 Ophiuchi Bab components are orbiting each other with a period of 2.9655 days. Both outer and inner orbits are nearly circular and, probably, coplanar (in

keeping with a general tendency of close triple systems).

V1054 Ophiuchi A-Bab pair is also visually resolved (for nearly 50 years it was the shortest-period resolved by visual means binary, since its binarity was discovered by G. P. Kuiper in 1934), whereas V1054 Ophiuchi Ba-Bb pair is still unresolved).At least it was not resolved by 2001.

=Gliese 643=

The projected separation of Gliese 643 from V1054 Ophiuchi A-Bab is 72 arcsec, corresponding at 21.05 light-years to 465 AU.

=V1054 Ophiuchi C (vB 8)=

vB 8 is the smallest, faintest, and most separated component of the V1054 Ophiuchi system. The projected separation of the red dwarf from the primary triple system is about 220 arcsec, corresponding at 21.05 light-years to 1420 a.u. Since it is only three times larger than the projected separation between Gliese 643 and V1054 Ophiuchi A-Bab, and such a small ratio should render the triple system dynamically unstable, it was suggested that the real separation of V1054 Ophiuchi C from V1054 Ophiuchi A-Bab is much larger, at least by a factor of two, i. e. at least 2840 a.u.

In 1984, the apparent detection of an infrared source near vB 8 suggested it had a low mass companion. The low mass of this candidate led to speculation that it may be a brown dwarf; the first such to be detected. This discovery was later found to be spurious, but it produced much interest in this class of astronomical object.{{cite book

| title=New Light on Dark Stars: Red Dwarfs, Low-Mass Stars, Brown Dwarfs

| series=Astronomy and Planetary Sciences

| first1=Neill I. | last1=Reid | first2=Suzanne L. | last2=Hawley

| date=27 November 2013

| publisher=Springer Science & Business Media, 2013

| url=https://books.google.com/books?id=04_aBwAAQBAJ&pg=PA344

| isbn=978-1447136637 | page=344 }}

Notes

References

{{reflist|colwidth=30em|refs=

{{cite simbad | title= HD 152751 | access-date=2019-03-25 }}

{{cite simbad | title=GJ 643}}

{{cite simbad | title=VB 8}}

{{Cite Gaia DR3|4339465360510320128}}

{{Cite Gaia DR3|4339417394313320192}}

{{cite journal

| title=The M-dwarf Ultraviolet Spectroscopic Sample. I. Determining Stellar Parameters for Field Stars

| last1=Pineda | first1=J. Sebastian | last2=Youngblood | first2=Allison

| last3=France | first3=Kevin

| journal=The Astrophysical Journal

| volume=918 | issue=1 | id=40 | pages=23 | date=September 2021

| doi=10.3847/1538-4357/ac0aea | arxiv=2106.07656

| bibcode=2021ApJ...918...40P | s2cid=235435757 | doi-access=free }}

{{cite journal |last1=Dal |first1=H. A. |last2=Evren |first2=S. |title=A New Method for Classifying Flares of UV Ceti Type Stars: Differences Between Slow and Fast Flares |journal=The Astronomical Journal |date=August 2010 |volume=140 |issue=2 |pages=483–489 |doi=10.1088/0004-6256/140/2/483 |url=https://ui.adsabs.harvard.edu/abs/2010AJ....140..483D |access-date=4 February 2022|arxiv=1206.5791 |bibcode=2010AJ....140..483D |s2cid=119308060 }}

[http://vizier.cfa.harvard.edu/viz-bin/VizieR?-source=I/238 VizieR, Yale Trigonometric Parallaxes, Fourth Edition (van Altena+ 1995)]

{{cite journal

|last1=Ségransan |first1=Damien

|last2=Delfosse |first2=Xavier

|last3=Forveille |first3=Thierry

|last4=Beuzit |first4=Jean-Luc

|last5=Udry |first5=Stéphane

|last6=Perrier |first6=Christian

|last7=Mayor |first7=Michel

|year=2000

|title=Accurate masses of very low mass stars. III. 16 new or improved masses

|journal=Astronomy and Astrophysics

|volume=364 | pages=665–673

|bibcode=2000A&A...364..665S

|arxiv = astro-ph/0010585 }}

{{Cite journal |last1=Kemmer |first1=J. |last2=Lafarga |first2=M. |last3=Fuhrmeister |first3=B. |last4=Shan |first4=Y. |last5=Schöfer |first5=P. |last6=Jeffers |first6=S. V. |last7=Caballero |first7=J. A. |last8=Quirrenbach |first8=A. |last9=Amado |first9=P. J. |date=2025-04-11 |title=The CARMENES search for exoplanets around M dwarfs. Cluster analysis of signals from spectral activity indicators to search for shared periods |journal=Astronomy and Astrophysics |volume=697 |doi=10.1051/0004-6361/202347056 |arxiv=2504.08363|bibcode=2025A&A...697A.225K }}

{{cite journal

| last=Mazeh |first=Tsevi

|author2=Latham, David W. |author3=Goldberg, Elad |author4=Torres, Guillermo |author5=Stefanik, Robert P. |author6=Henry, Todd J. |author7=Zucker, Shay |author8=Gnat, Orly |author9= Ofek, Eran O.

| year=2001

| title=Studies of multiple stellar systems - IV. The triple-lined spectroscopic system V1054 Ophiuchi

| journal=Monthly Notices of the Royal Astronomical Society

| volume=325 |issue=1

| pages=343–357

| bibcode=2001MNRAS.325..343M

| doi=10.1046/j.1365-8711.2001.04419.x

|doi-access=free

|arxiv = astro-ph/0102451 |s2cid=16472347

}}

{{cite journal |first1=Céline |last1=Reylé |first2=Kevin |last2=Jardine |first3=Pascal |last3=Fouqué |first4=Jose A. |last4=Caballero |first5=Richard L. |last5=Smart |first6=Alessandro |last6=Sozzetti |date=30 April 2021 |title=The 10 parsec sample in the Gaia era |journal=Astronomy & Astrophysics |volume=650 |issue= |pages=A201 |doi=10.1051/0004-6361/202140985 |arxiv=2104.14972 |bibcode=2021A&A...650A.201R |s2cid=233476431}} Data available at https://gruze.org/10pc/ {{Webarchive|url=https://web.archive.org/web/20230312171927/http://gruze.org/10pc/ |date=12 March 2023 }}

{{cite journal |bibcode=2012AstL...38..331A |title=XHIP: An extended hipparcos compilation |last1=Anderson |first1=E. |last2=Francis |first2=Ch. |journal=Astronomy Letters |date=2012 |volume=38 |issue=5 |page=331 |doi=10.1134/S1063773712050015 |arxiv=1108.4971 }}

{{cite journal |bibcode=2004A&A...424..727P |title=SB9: The ninth catalogue of spectroscopic binary orbits |last1=Pourbaix |first1=D. |last2=Tokovinin |first2=A. A. |last3=Batten |first3=A. H. |last4=Fekel |first4=F. C. |last5=Hartkopf |first5=W. I. |last6=Levato |first6=H. |last7=Morrell |first7=N. I. |last8=Torres |first8=G. |last9=Udry |first9=S. |journal=Astronomy and Astrophysics |date=2004 |volume=424 |page=727 |doi=10.1051/0004-6361:20041213 |arxiv=astro-ph/0406573 }}

}}

{{Stars of Ophiuchus}}

{{DEFAULTSORT:V1054 Ophiuchi}}

Category:Ophiuchus

5

Category:M-type main-sequence stars

0644

Ophiuchi, V1054

152751

082817

BD-08 4352

0629 30