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Coordinates: Sky map 22h 56m 24.0533s, −31° 33′ 56.0351″
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{{Short description|Star in the constellation Piscis Austrinus}}
{{Redirect|Fomalhaut B|the extrasolar planet candidate|Fomalhaut b}}
{{Redirect|Fomalhaut B|the former exoplanet candidate|Fomalhaut b}}
{{Starbox begin
{{Starbox begin
| name=TW Piscis Austrini }}
| name=TW Piscis Austrini
}}
{{Starbox image
| image=
{{Location mark
|image=Piscis Austrinus constellation map.svg|alt=|float=center|width=280
|label=|position=right
|mark=Red circle.svg|mark_width=10|mark_link=TW Piscis Austrini
|x=178|y=436
}}
|caption=Location of TW Piscis Austrini (circled)
}}
{{Starbox observe
{{Starbox observe
| epoch=J2000
| epoch = J2000
| constell=[[Piscis Austrinus]]
| ra={{RA|22|56|24.05327}}<ref name=aaa474_2_653/>
| dec={{DEC|−31|33|56.0351}}<ref name=aaa474_2_653/>
| ra = {{RA|22|56|24.05256}}<ref name="GaiaDR3"/>
| appmag_v=6.48<ref name="SIMBAD">{{cite web
| dec = {{DEC|−31|33|56.0306}}<ref name="GaiaDR3"/>
| appmag_v = 5.44–6.51<ref name=gcvs/>
| title=V* TW PsA -- Variable of BY Dra type | work=SIMBAD
}}
| publisher=Centre de Données astronomiques de Strasbourg
| url=http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=GJ+879&submit=SIMBAD+search
| accessdate=2010-01-20 }}</ref>
| constell=[[Piscis Austrinus]] }}
{{Starbox character
{{Starbox character
| class=K5Vp<ref name=aaa505_1_205/>
| class=K5Vp<ref name=aaa505_1_205/>
| b-v=1.10<ref name="clpl4">{{cite journal
| b-v=1.10<ref name=clpl4/>
| u-b=1.02<ref name=clpl4/>
| author=Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z.
| variable=[[BY Draconis variable|BY Draconis]]<ref name=gcvs/>
| title=UBVRIJKL photometry of the bright stars
}}
| journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | year=1966
| bibcode=1966CoLPL...4...99J }}</ref>
| u-b=1.02<ref name="clpl4" />
| variable=[[BY Draconis variable|BY Draconis]] }}
{{Starbox astrometry
{{Starbox astrometry
| radial_v=+6<ref name="SIMBAD" />
| radial_v = {{val|+6.79|0.12}}<ref name="GaiaDR3"/>
| prop_mo_ra=−331.11<ref name=aaa474_2_653/>
| prop_mo_ra = {{val|330.203}}
| prop_mo_dec=−158.98<ref name=aaa474_2_653/>
| prop_mo_dec = {{val|−158.602}}
| pm_footnote = <ref name="GaiaDR3"/>
| parallax=131.42
| parallax = 131.5525
| p_error=0.62
| p_error = 0.0275
| parallax_footnote=<ref name=aaa474_2_653/>
| absmag_v=7.08<ref name="age_mam"/> }}
| parallax_footnote = <ref name="GaiaDR3"/>
| absmag_v = 7.08<ref name="age_mam"/>
}}
{{Starbox detail
{{Starbox detail
| mass={{nowrap|0.725 ± 0.036}}<ref name=aaa505_1_205/>
| source=<ref name=Gomes2021/>
| radius={{nowrap|0.629 ± 0.051}}<ref name=aaa505_1_205 />
| mass={{val|0.704|0.016}}
| radius={{val|0.658|0.009}}
| luminosity=0.19<ref name="age_mam"/>
| luminosity=0.19<ref name="age_mam"/>
| temperature={{nowrap|4,711 ± 134}}<ref name=aaa505_1_205/>
| temperature={{val|4610|67|fmt=commas}}
| metal_fe={{val|-0.07|0.03}}
| metal=
| rotation=
| rotation=10.3<ref name=Mamajek/> days
| rotational_velocity=2.93<ref name=aaa505_1_205/>
| rotational_velocity=2.93<ref name=aaa505_1_205/>
| age=4.4 × 10<sup>8</sup><ref name="age_mam"/> }}
| age_myr=440<ref name="age_mam"/>
}}
{{Starbox catalog
{{Starbox catalog
| names=TW PsA, [[Henry L. Giclas catalogue|Gl]] 879, [[Harvard Revised catalogue|HR]] 8721, [[Cordoba Durchmusterung|CD]] -32°17321, [[Henry Draper catalogue|HD]] 216803, [[Luyten Two-Tenths catalogue|LTT]] 9283, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 5562.00, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 214197, CP(D)-32 6550, [[Hipparcos catalogue|HIP]] 113283. }}
| names=TW PsA, [[Gliese Catalogue of Nearby Stars|Gl]] 879, [[Harvard Revised catalogue|HR]] 8721, [[Cordoba Durchmusterung|CD]]−32°17321, [[Henry Draper catalogue|HD]] 216803, [[Luyten Two-Tenths catalogue|LTT]] 9283, [[General Catalogue of Trigonometric Parallaxes|GCTP]] 5562.00, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]] 214197, CP(D)−32°6550, [[Hipparcos catalogue|HIP]] 113283<ref name=SIMBAD/>
}}
{{Starbox reference
{{Starbox reference
| Simbad = HD+216803
| Simbad = HD+216803
Line 47: Line 58:
}}
}}
{{Starbox end}}
{{Starbox end}}
'''TW Piscis Austrini''' (also Fomalhaut B) is a dwarf [[star]] in the [[constellation]] [[Piscis Austrinus]]. It lies relatively close to the [[Sun]], at an estimated distance of 24.9 [[light year]]s.
'''TW Piscis Austrini''' (also known as Fomalhaut B) is a [[main sequence]] star in the [[constellation]] [[Piscis Austrinus]]. It lies relatively close to the [[Sun]], at an estimated distance of {{convert|24.8|ly|pc|lk=on|abbr=off}}.
To an observer on Earth the star is visually separated from its larger companion [[Fomalhaut]] (A) by 2 degrees—the width of four [[full moon]]s.<ref name=skyandtelescope2014-10-01/>


[[File:TWPsALightCurve.png|thumb|left| A [[Photometric_system#Photometric_letters|visual band]] [[light curve]] for TW Piscis Austrini, adapted from Busko and Torres (1978).<ref name="Busko"/> The error bar shown on the left-most point applies to all points.]]
The TW in the name is astronomical nomenclature for a [[variable star]]. This is a [[flare star]] of the type known as a [[BY Draconis variable]]. It varies slightly in [[apparent magnitude]], ranging from 6.44 to 6.49 over a 10.3 day period. While smaller than the [[Sun]], it is relatively large for a flare star. Most flare stars are red [[stellar classification|M-type]] dwarfs.
The name TW Piscis Austrini is a [[variable star designation]]. This is a [[variable star]] of the type known as a [[BY Draconis variable]], with surface brightness variations causing the changes as the star rotates. It varies slightly in [[apparent magnitude]], ranging from 6.44 to 6.51 over a 10.3-day period.<ref name=gcvs/>


TW Piscis Austrini lies within a light-year of Fomalhaut.<ref name=schaaf2008/> Due to sharing the same [[proper motion]], and the same estimated age of approximately 440 ± 40 million years, astronomers now consider them to be elements of a multiple [[star system]].<ref name="age_mam"/> A third star, dimmer and more widely separated, [[Fomalhaut C]], gives the system the widest visual separation, to observers from Earth, at approximately 6 degrees.<ref name=skyandtelescope2014-10-01/>
TW Piscis Austrini lies within a [[light year]] of the much brighter star [[Fomalhaut]],<ref>p. 237, ''The Brightest Stars: Discovering The Universe Through The Sky's Most Brilliant Stars'', Fred Schaaf, Hoboken, NJ: John Wiley & Sons, Inc., 2008, ISBN 978-0-471-70410-2.</ref> and the two may be travelling companions that share a common motion through space.
==Planetary system==
In 2019, an [[exoplanet]] candidate around Fomalhaut B was detected by [[astrometry]], but this remains unconfirmed.<ref name=space2019-09-23/><ref name=AstronomicalJournal2019-10-07/>


{{OrbitboxPlanet begin
A 2012 study<ref name="age_mam"/> showed that TW PsA and [[Fomalhaut]] are approximately only 0.28 parsecs (57,000 AU) apart, and share a space velocity within 0.1±0.5&nbsp;km/s, consistent with constituting a physical binary system. Independent age estimates for [[Fomalhaut]] and TW PsA yield similar results, and the age for the system is 440±40 million years.<ref name="age_mam"/>
| name = Fomalhaut B

In 2019 NASA's [[Transiting Exoplanet Survey Satellite]] space telescope found a exoplanet candidate around Fomalhaut B.<ref name=space2019-09-23/><ref name=AstronomicalJournal2019-10-07/>
| table_ref = <ref name=AstronomicalJournal2019-10-07/>
| period_unit = year
}}
{{OrbitboxPlanet hypothetical
| exoplanet = b
| period = {{val|25|52|21}}
| mass = {{val|1.2|0.7|0.6}}
}}
{{Orbitbox end}}


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


<ref name="GaiaDR3">{{Cite Gaia DR3|6604147121141267712}}</ref>
<ref name=age_mam>{{Cite journal | last1=Mamajek | first1=E.E. | title=On the Age and Binarity of Fomalhaut | journal=Astrophysical Journal Letters | volume=754 | issue=2 |date=August 2012 | pages=L20 | doi=10.1088/2041-8205/754/2/L20 | bibcode=2012ApJL..754...20M | arxiv=1206.6353}}</ref>


<ref name=aaa474_2_653>{{citation | last1=van Leeuwen | first1=F. | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 |date=November 2007 | pages=653–664 | doi=10.1051/0004-6361:20078357 | bibcode=2007A&A...474..653V | arxiv=0708.1752 }}</ref>
<ref name="Busko">{{cite journal |last1=Busko |first1=I. C. |last2=Torres |first2=C. A. O. |title=Flare activity by BY Draconis stars |journal=Astronomy and Astrophysics |date=March 1978 |volume=64 |pages=153–160 |bibcode=1978A&A....64..153B |url=https://ui.adsabs.harvard.edu/abs/1978A&A....64..153B |access-date=23 February 2022}}</ref>


<ref name=schaaf2008>{{cite book|author=Fred Schaaf|title=The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars|url=https://books.google.com/books?id=9LT1q0Il3-YC|date=31 March 2008|publisher=Wiley|isbn=978-0-470-24917-8}}</ref>
<ref name=aaa505_1_205>{{citation | display-authors=1 | last1=Demory | first1=B.-O. | last2=Ségransan | first2=D. | last3=Forveille | first3=T. | last4=Queloz | first4=D. | last5=Beuzit | first5=J.-L. | last6=Delfosse | first6=X. | last7=di Folco | first7=E. | last8=Kervella | first8=P. | last9=Le Bouquin | first9=J.-B. |date=October 2009 | title=Mass-radius relation of low and very low-mass stars revisited with the VLTI | journal=Astronomy and Astrophysics | volume=505 | issue=1 | pages=205–215 | doi=10.1051/0004-6361/200911976 | bibcode=2009A&A...505..205D |arxiv = 0906.0602 }}</ref>

<ref name=age_mam>{{Cite journal | last1=Mamajek | first1=E.E. | title=On the Age and Binarity of Fomalhaut | journal=Astrophysical Journal Letters | volume=754 | issue=2 |date=August 2012 | pages=L20 | doi=10.1088/2041-8205/754/2/L20 | arxiv=1206.6353| bibcode=2012ApJ...754L..20M | s2cid=119191190 }}</ref>

<ref name=aaa505_1_205>{{cite journal
| title=Mass-radius relation of low and very low-mass stars revisited with the VLTI
| journal=Astronomy and Astrophysics | volume=505 | issue=1
| date=October 2009 | pages=205–215
| doi=10.1051/0004-6361/200911976
| bibcode=2009A&A...505..205D |arxiv = 0906.0602
|last1=Demory |first1=Brice-Olivier
|last2=Ségransan |first2=Damien
|last3=Forveille |first3=Thierry
|last4=Queloz |first4=Didier
|last5=Beuzit |first5=Jean-Luc
|last6=Delfosse |first6=Xavier
|last7=Di Folco |first7=Emmanuel
|last8=Kervella |first8=Pierre
|last9=Le Bouquin |first9=Jean-Baptiste
|last10=Perrier |first10=Christian
|last11=Benisty |first11=Myriam
|last12=Duvert |first12=Gilles
|last13=Hofmann |first13=Karl-Heinz
|last14=Lopez |first14=Bruno
|last15=Petrov |first15=Romain
|s2cid=14786643
}}</ref>


<ref name=space2019-09-23>
<ref name=space2019-09-23>
Line 70: Line 120:
| url = https://www.space.com/fomalhaut-autumn-star-skywatching.html
| url = https://www.space.com/fomalhaut-autumn-star-skywatching.html
| title = Fomalhaut, 'Royal' Star of Autumn, Swims with the Southern Fish
| title = Fomalhaut, 'Royal' Star of Autumn, Swims with the Southern Fish
| work = [[Space magazine]]
| work = [[Space.com]]
| author = Joe Rao
| author = Joe Rao
| date = 2019-09-23
| date = 2019-09-23
Line 76: Line 126:
| archivedate =
| archivedate =
| accessdate = 2020-06-13
| accessdate = 2020-06-13
| url-status = live
| quote = Believe it or not, an extrasolar planet might also be circling TW Piscis Austrini. NASA's Transiting Exoplanet Survey Satellite (TESS), a space telescope that's searching for planets around the brightest stars in Earth's night sky, recently found a possible candidate circling this star. It's almost the same size as our Earth, and orbits the star about every 10 days at a distance of 7.5 million miles from it.
| quote = Believe it or not, an extrasolar planet might also be circling TW Piscis Austrini. NASA's Transiting Exoplanet Survey Satellite (TESS), a space telescope that's searching for planets around the brightest stars in Earth's night sky, recently found a possible candidate circling this star. It's almost the same size as our Earth, and orbits the star about every 10 days at a distance of 7.5 million miles from it.
}}
}}
Line 103: Line 152:
| first8 = Bruce
| first8 = Bruce
| date = 7 October 2019
| date = 7 October 2019
|volume = 158
| eprint = 1910.02965
|issue = 6
| class = astro-ph.EP
|page = 225
| arxiv = 1910.02965
| doi = 10.3847/1538-3881/ab4c9b
|bibcode = 2019AJ....158..225D
|s2cid = 203902656
|doi-access = free
}}
}}
</ref>
</ref>

<ref name=skyandtelescope2014-10-01>
{{cite news
| url = https://skyandtelescope.org/astronomy-news/fomalhaut-falls-amazing-triple-star10012014/
| title = Fomalhaut: A crazy-wide triple stat
| work = [[Sky & Telescope]]
| author = Bob King
| date = 2014-10-01
| archiveurl =
| archivedate =
| accessdate = 2020-06-13
| quote = Though it may appear isolated in the barren October sky, Fomalhaut has company. It feels the gravitational tug of the magnitude +6.5 star TW Piscis Austrini, 2° to the south. Both are 25 light-years distant and move in tandem across space, partaking of the same proper motion. They form a true double star with an actual separation of 5.5 trillion miles, or 0.91 light-year.
}}
}}
</ref>


<ref name=SIMBAD>{{cite web
== External links ==
| title=V* TW PsA -- Variable of BY Dra type | work=SIMBAD
| publisher=Centre de Données astronomiques de Strasbourg
| url=http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=GJ+879&submit=SIMBAD+search
| accessdate=2010-01-20 }}</ref>

<ref name=clpl4>{{cite journal
| title=UBVRIJKL photometry of the bright stars
| journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | year=1966
| page=99
| bibcode=1966CoLPL...4...99J | last1=Johnson | first1=H. L. | last2=Mitchell | first2=R. I. | last3=Iriarte | first3=B. | last4=Wisniewski | first4=W. Z. }}</ref>

<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|pages=B/gcvs|display-authors=etal|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}</ref>

<ref name=Mamajek>{{cite journal
| author1=Mamajek, Eric E. | display-authors=etal
| title=The Solar Neighborhood. XXX. Fomalhaut C
| journal=The Astronomical Journal
| volume=146 | issue=6 | pages=154–163 | date=2013
| bibcode=2013AJ....146..154M
| doi=10.1088/0004-6256/146/6/154
| arxiv=1310.0764|s2cid=67821813}}</ref>


<ref name=Gomes2021>{{Cite journal |last=Gomes da Silva |first=J. |last2=Santos |first2=N. C. |last3=Adibekyan |first3=V. |last4=Sousa |first4=S. G. |last5=Campante |first5=T. L. |last6=Figueira |first6=P. |last7=Bossini |first7=D. |last8=Delgado-Mena |first8=E. |last9=Monteiro |first9=M. J. P. F. G. |last10=de Laverny |first10=P. |last11=Recio-Blanco |first11=A. |last12=Lovis |first12=C. |date=2021-02-01 |title=Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample. I. A catalogue of homogeneous chromospheric activity |url=https://ui.adsabs.harvard.edu/abs/2021A&A...646A..77G |journal=Astronomy and Astrophysics |volume=646 |pages=A77 |doi=10.1051/0004-6361/202039765 |issn=0004-6361|arxiv=2012.10199 }} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/646/A77&Star=TW%20PsA Fomalhaut B's database entry] at [[VizieR]].</ref>

}}

==External links==
* [http://www.solstation.com/stars/tw-psa.htm TW Piscis Austrini] at SolStation.
* [http://www.solstation.com/stars/tw-psa.htm TW Piscis Austrini] at SolStation.
{{Sky|22|56|24.0533|-|31|33|56.0351|24.8}}
{{Nearest star systems|6}}
{{Nearest star systems|6}}
{{Stars of Piscis Austrinus}}
{{Stars of Piscis Austrinus}}
{{Fomalhaut}}

{{DEFAULTSORT:TW Piscis Austrini}}
[[Category:Piscis Austrinus]]
[[Category:Piscis Austrinus]]
[[Category:K-type main-sequence stars]]
[[Category:K-type main-sequence stars]]
[[Category:BY Draconis variables]]
[[Category:BY Draconis variables]]
[[Category:Objects within 100 ly of Earth]]
[[Category:Objects with variable star designations|Piscis Austrini, TW]]
[[Category:Objects named with variable star designations|Piscis Austrini, TW]]
[[Category:Henry Draper Catalogue objects|216803]]
[[Category:Henry Draper Catalogue objects|216803]]
[[Category:Hipparcos objects|113283]]
[[Category:Bright Star Catalogue objects|8721]]
[[Category:Gliese and GJ objects|0879]]
[[Category:Durchmusterung objects|CD-32 17321]]
[[Category:Fomalhaut]]

Latest revision as of 23:47, 15 July 2024

"Fomalhaut B" redirects here. For the former exoplanet candidate, see Fomalhaut b.
TW Piscis Austrini
Location of TW Piscis Austrini (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Piscis Austrinus
Right ascension 22h 56m 24.05256s[1]
Declination −31° 33′ 56.0306″[1]
Apparent magnitude (V) 5.44–6.51[2]
Characteristics
Spectral type K5Vp[3]
U−B color index 1.02[4]
B−V color index 1.10[4]
Variable type BY Draconis[2]
Astrometry
Radial velocity (Rv)+6.79±0.12[1] km/s
Proper motion (μ) RA: 330.203 mas/yr[1]
Dec.: −158.602 mas/yr[1]
Parallax (π)131.5525 ± 0.0275 mas[1]
Distance24.793 ± 0.005 ly
(7.602 ± 0.002 pc)
Absolute magnitude (MV)7.08[5]
Details[6]
Mass0.704±0.016 M☉
Radius0.658±0.009 R☉
Luminosity0.19[5] L☉
Temperature4,610±67 K
Metallicity [Fe/H]−0.07±0.03 dex
Rotation10.3[7] days
Rotational velocity (v sin i)2.93[3] km/s
Age440[5] Myr
Other designations
TW PsA, Gl 879, HR 8721, CD−32°17321, HD 216803, LTT 9283, GCTP 5562.00, SAO 214197, CP(D)−32°6550, HIP 113283[8]
Database references
SIMBADdata
ARICNSdata

TW Piscis Austrini (also known as Fomalhaut B) is a main sequence star in the constellation Piscis Austrinus. It lies relatively close to the Sun, at an estimated distance of 24.8 light-years (7.6 parsecs). To an observer on Earth the star is visually separated from its larger companion Fomalhaut (A) by 2 degrees—the width of four full moons.[9]

A visual band light curve for TW Piscis Austrini, adapted from Busko and Torres (1978).[10] The error bar shown on the left-most point applies to all points.

The name TW Piscis Austrini is a variable star designation. This is a variable star of the type known as a BY Draconis variable, with surface brightness variations causing the changes as the star rotates. It varies slightly in apparent magnitude, ranging from 6.44 to 6.51 over a 10.3-day period.[2]

TW Piscis Austrini lies within a light-year of Fomalhaut.[11] Due to sharing the same proper motion, and the same estimated age of approximately 440 ± 40 million years, astronomers now consider them to be elements of a multiple star system.[5] A third star, dimmer and more widely separated, Fomalhaut C, gives the system the widest visual separation, to observers from Earth, at approximately 6 degrees.[9]

Planetary system

[edit]

In 2019, an exoplanet candidate around Fomalhaut B was detected by astrometry, but this remains unconfirmed.[12][13]

The Fomalhaut B planetary system[13]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
b (unconfirmed) 1.2+0.7
−0.6 MJ 		— 25+52
−21 		— — —

References

[edit]
  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  3. ^ a b Demory, Brice-Olivier; Ségransan, Damien; Forveille, Thierry; Queloz, Didier; Beuzit, Jean-Luc; Delfosse, Xavier; Di Folco, Emmanuel; Kervella, Pierre; Le Bouquin, Jean-Baptiste; Perrier, Christian; Benisty, Myriam; Duvert, Gilles; Hofmann, Karl-Heinz; Lopez, Bruno; Petrov, Romain (October 2009). "Mass-radius relation of low and very low-mass stars revisited with the VLTI". Astronomy and Astrophysics. 505 (1): 205–215. arXiv:0906.0602. Bibcode:2009A&A...505..205D. doi:10.1051/0004-6361/200911976. S2CID 14786643.
  4. ^ a b Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  5. ^ a b c d Mamajek, E.E. (August 2012). "On the Age and Binarity of Fomalhaut". Astrophysical Journal Letters. 754 (2): L20. arXiv:1206.6353. Bibcode:2012ApJ...754L..20M. doi:10.1088/2041-8205/754/2/L20. S2CID 119191190.
  6. ^ Gomes da Silva, J.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Campante, T. L.; Figueira, P.; Bossini, D.; Delgado-Mena, E.; Monteiro, M. J. P. F. G.; de Laverny, P.; Recio-Blanco, A.; Lovis, C. (2021-02-01). "Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample. I. A catalogue of homogeneous chromospheric activity". Astronomy and Astrophysics. 646: A77. arXiv:2012.10199. doi:10.1051/0004-6361/202039765. ISSN 0004-6361. Fomalhaut B's database entry at VizieR.
  7. ^ Mamajek, Eric E.; et al. (2013). "The Solar Neighborhood. XXX. Fomalhaut C". The Astronomical Journal. 146 (6): 154–163. arXiv:1310.0764. Bibcode:2013AJ....146..154M. doi:10.1088/0004-6256/146/6/154. S2CID 67821813.
  8. ^ "V* TW PsA -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-01-20.
  9. ^ a b Bob King (2014-10-01). "Fomalhaut: A crazy-wide triple stat". Sky & Telescope. Retrieved 2020-06-13. Though it may appear isolated in the barren October sky, Fomalhaut has company. It feels the gravitational tug of the magnitude +6.5 star TW Piscis Austrini, 2° to the south. Both are 25 light-years distant and move in tandem across space, partaking of the same proper motion. They form a true double star with an actual separation of 5.5 trillion miles, or 0.91 light-year.
  10. ^ Busko, I. C.; Torres, C. A. O. (March 1978). "Flare activity by BY Draconis stars". Astronomy and Astrophysics. 64: 153–160. Bibcode:1978A&A....64..153B. Retrieved 23 February 2022.
  11. ^ Fred Schaaf (31 March 2008). The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars. Wiley. ISBN 978-0-470-24917-8.
  12. ^ Joe Rao (2019-09-23). "Fomalhaut, 'Royal' Star of Autumn, Swims with the Southern Fish". Space.com. Retrieved 2020-06-13. Believe it or not, an extrasolar planet might also be circling TW Piscis Austrini. NASA's Transiting Exoplanet Survey Satellite (TESS), a space telescope that's searching for planets around the brightest stars in Earth's night sky, recently found a possible candidate circling this star. It's almost the same size as our Earth, and orbits the star about every 10 days at a distance of 7.5 million miles from it.
  13. ^ a b De Rosa, Robert J.; Esposito, Thomas M.; Hirsch, Lea A.; Nielsen, Eric L.; Marley, Mark S.; Kalas, Paul; Wang, Jason J.; Macintosh, Bruce (7 October 2019). "The Possible Astrometric Signature of a Planetary-mass Companion to the Nearby Young Star TW Piscis Austrini (Fomalhaut B): Constraints from Astrometry, Radial Velocities, and Direct Imaging". Astronomical Journal. 158 (6): 225. arXiv:1910.02965. Bibcode:2019AJ....158..225D. doi:10.3847/1538-3881/ab4c9b. S2CID 203902656.
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