Jump to content

DS Tucanae: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
(2 intermediate revisions by one other user not shown)
Line 67: Line 67:
{{Starbox end}}
{{Starbox end}}


'''DS Tucanae''' ('''HD 222259''') is a [[binary star]] system 144 [[light year]]s away in the constellation of [[Tucana]]. It has an [[apparent visual magnitude]] of 8.5,<ref name="Newton et al." /> and is a [[RS Canum Venaticorum variable|RS Canum Venaticorum]] variable.<ref name=gcvs>{{Cite journal|last1=Samus'|first1=N. N.|last2=Goranskii|first2=V. P.|last3=Durlevich|first3=O. V.|last4=Zharova|first4=A. V.|last5=Kazarovets|first5=E. V.|last6=Kireeva|first6=N. N.|last7=Pastukhova|first7=E. N.|last8=Williams|first8=D. B.|last9=Hazen|first9=M. L.|date=July 2003|title=An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates|journal= Astronomy Letters|language=en|volume=29|issue=7|pages=468–479|doi=10.1134/1.1589864|issn=1063-7737|bibcode=2003AstL...29..468S|s2cid=16299532}}</ref> The system is notable for being young as a member of the 45 [[Myr]] old [[Tucana-Horologium association|Tucana-Horologium moving group]]<ref>{{Cite journal|last1=Zuckerman|first1=B.|last2=Webb|first2=R. A.|date=2000-06-01|title=Identification of a Nearby Stellar Association in theHipparcos Catalog: Implications for Recent, Local Star Formation|journal=The Astrophysical Journal|language=en|volume=535|issue=2|pages=959|doi=10.1086/308897|issn=0004-637X|bibcode=2000ApJ...535..959Z|arxiv=astro-ph/0002461|s2cid=2485534}}</ref> and for the primary star hosting the confirmed [[exoplanet]] '''DS Tucanae Ab''', discovered by [[TESS Hunt for Young and Maturing Exoplanets|THYME]], using [[Transiting Exoplanet Survey Satellite|TESS]].<ref>{{Cite web|url=https://news.dartmouth.edu/news/2019/08/dartmouth-astronomer-leading-discovery-new-planet|title=Dartmouth Astronomer on Leading Discovery of a New Planet {{!}} Dartmouth News|last=Albright|first=Charlotte|date=|website=news.dartmouth.edu|access-date=2022-01-30}}</ref><ref name="Newton et al.">{{Cite journal|display-authors=1|last1=Newton|first1=Elisabeth R.|last2=Mann|first2=Andrew W.|last3=Tofflemire|first3=Benjamin M.|last4=Pearce|first4=Logan|last5=Rizzuto|first5=Aaron C.|last6=Vanderburg|first6=Andrew|last7=Martinez|first7=Raquel A.|last8=Wang|first8=Jason J.|last9=Ruffio|first9=Jean-Baptiste|last10=Kraus|first10=Adam L.|last11=Johnson|first11=Marshall C.|last12=Thao|first12= Pa Chia|last13=Wood|first13= Mackenna L.|last14=Rampalli|first14= Rayna|last15=Nielsen|first15= Eric L.|last16=Collins|first16= Karen A.|last17=Dragomir|first17= Diana|last18=Hellier|first18= Coel|last19=Anderson|first19= D. R.|last20=Barclay|first20= Thomas|last21=Brown|first21= Carolyn|last22=Feiden|first22= Gregory|last23=Hart|first23= Rhodes|last24=Isopi|first24= Giovanni|last25=Kielkopf|first25= John F.|last26=Mallia|first26= Franco|last27=Nelson|first27= Peter|last28=Rodriguez|first28= Joseph E.|last29=Stockdale|first29= Chris|last30=Waite|first30= Ian A.|last31=Wright|first31= Duncan J.|last32=Lissauer|first32= Jack J.|last33=Ricker|first33= George R.|last34=Vanderspek|first34= Roland|last35=Latham|first35= David W.|last36=Seager|first36= S.|last37=Winn|first37= Joshua N.|last38=Jenkins|first38= Jon M.|last39=Bouma|first39= Luke G.|last40=Burke|first40= Christopher J.|last41=Davies|first41= Misty|last42=Fausnaugh|first42= Michael|last43=Li|first43= Jie|last44=Morris|first44= Robert L.|last45=Mukai|first45= Koji|last46=Villaseñor|first46= Joel|last47=Villeneuva|first47= Steven|last48=De Rosa|first48= Robert J.|last49=Macintosh|first49= Bruce|last50=Mengel|first50= Matthew W.|last51=Okumura|first51= Jack|last52=Wittenmyer|first52= Robert A.|date=July 2019|title=TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana-Horologium Association|journal= The Astrophysical Journal Letters|language=en|volume=880|issue=1|pages=L17|doi=10.3847/2041-8213/ab2988 | arxiv=1906.10703 |issn=0004-637X|bibcode=2019ApJ...880L..17N|hdl=1721.1/124722|s2cid=195658207|hdl-access=free}}</ref><ref name="Benatti et al.">{{Cite journal|last1=Benatti|first1=S.|last2=Nardiello|first2=D.|last3=Malavolta|first3=L.|last4=Desidera|first4=S.|last5=Borsato|first5=L.|last6=Nascimbeni|first6=V.|last7=Damasso|first7=M.|last8=D'Orazi|first8=V.|last9=Mesa|first9=D.|last10=Messina|first10=S.|last11=Esposito|first11=M.|last12=Bignamini|first12=A.|last13=Claudi|first13=R.|last14=Covino|first14=E.|last15=Lovis|first15=C.|last16=Sabotta|first16=S.|date=October 2019|title=A possibly inflated planet around the bright young star DS Tucanae A|journal= Astronomy & Astrophysics|language=en|volume=630|pages=A81|doi=10.1051/0004-6361/201935598|issn=0004-6361|bibcode=2019A&A...630A..81B|arxiv=1904.01591|s2cid=102486551}}</ref><ref>{{Cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=DS+Tuc+A+b&type=CONFIRMED_PLANET|title=DS Tuc A b|website=exoplanetarchive.ipac.caltech.edu|access-date=2019-12-18}}</ref>
'''DS Tucanae''' ('''HD 222259''') is a [[binary star]] system 144 [[light year]]s away in the constellation of [[Tucana]]. It has an [[apparent visual magnitude]] of 8.5,<ref name="Newton et al." /> and is a [[RS Canum Venaticorum variable|RS Canum Venaticorum]] variable.<ref name=gcvs>{{Cite journal|last1=Samus'|first1=N. N.|last2=Goranskii|first2=V. P.|last3=Durlevich|first3=O. V.|last4=Zharova|first4=A. V.|last5=Kazarovets|first5=E. V.|last6=Kireeva|first6=N. N.|last7=Pastukhova|first7=E. N.|last8=Williams|first8=D. B.|last9=Hazen|first9=M. L.|date=July 2003|title=An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates|journal= Astronomy Letters|language=en|volume=29|issue=7|pages=468–479|doi=10.1134/1.1589864|issn=1063-7737|bibcode=2003AstL...29..468S|s2cid=16299532}}</ref> The system is notable for being young as a member of the 45 [[Myr]] old [[Tucana-Horologium association|Tucana-Horologium moving group]]<ref>{{Cite journal|last1=Zuckerman|first1=B.|last2=Webb|first2=R. A.|date=2000-06-01|title=Identification of a Nearby Stellar Association in theHipparcos Catalog: Implications for Recent, Local Star Formation|journal=The Astrophysical Journal|language=en|volume=535|issue=2|pages=959|doi=10.1086/308897|issn=0004-637X|bibcode=2000ApJ...535..959Z|arxiv=astro-ph/0002461|s2cid=2485534}}</ref> and for the primary star hosting the confirmed [[exoplanet]] '''DS Tucanae Ab''', discovered by [[TESS Hunt for Young and Maturing Exoplanets|THYME]], using [[Transiting Exoplanet Survey Satellite|TESS]].<ref>{{Cite web|url=https://news.dartmouth.edu/news/2019/08/dartmouth-astronomer-leading-discovery-new-planet|title=Dartmouth Astronomer on Leading Discovery of a New Planet {{!}} Dartmouth News|last=Albright|first=Charlotte|date=14 August 2019|website=news.dartmouth.edu|access-date=2022-01-30}}</ref><ref name="Newton et al.">{{Cite journal|display-authors=1|last1=Newton|first1=Elisabeth R.|last2=Mann|first2=Andrew W.|last3=Tofflemire|first3=Benjamin M.|last4=Pearce|first4=Logan|last5=Rizzuto|first5=Aaron C.|last6=Vanderburg|first6=Andrew|last7=Martinez|first7=Raquel A.|last8=Wang|first8=Jason J.|last9=Ruffio|first9=Jean-Baptiste|last10=Kraus|first10=Adam L.|last11=Johnson|first11=Marshall C.|last12=Thao|first12= Pa Chia|last13=Wood|first13= Mackenna L.|last14=Rampalli|first14= Rayna|last15=Nielsen|first15= Eric L.|last16=Collins|first16= Karen A.|last17=Dragomir|first17= Diana|last18=Hellier|first18= Coel|last19=Anderson|first19= D. R.|last20=Barclay|first20= Thomas|last21=Brown|first21= Carolyn|last22=Feiden|first22= Gregory|last23=Hart|first23= Rhodes|last24=Isopi|first24= Giovanni|last25=Kielkopf|first25= John F.|last26=Mallia|first26= Franco|last27=Nelson|first27= Peter|last28=Rodriguez|first28= Joseph E.|last29=Stockdale|first29= Chris|last30=Waite|first30= Ian A.|last31=Wright|first31= Duncan J.|last32=Lissauer|first32= Jack J.|last33=Ricker|first33= George R.|last34=Vanderspek|first34= Roland|last35=Latham|first35= David W.|last36=Seager|first36= S.|last37=Winn|first37= Joshua N.|last38=Jenkins|first38= Jon M.|last39=Bouma|first39= Luke G.|last40=Burke|first40= Christopher J.|last41=Davies|first41= Misty|last42=Fausnaugh|first42= Michael|last43=Li|first43= Jie|last44=Morris|first44= Robert L.|last45=Mukai|first45= Koji|last46=Villaseñor|first46= Joel|last47=Villeneuva|first47= Steven|last48=De Rosa|first48= Robert J.|last49=Macintosh|first49= Bruce|last50=Mengel|first50= Matthew W.|last51=Okumura|first51= Jack|last52=Wittenmyer|first52= Robert A.|date=July 2019|title=TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana-Horologium Association|journal= The Astrophysical Journal Letters|language=en|volume=880|issue=1|pages=L17|doi=10.3847/2041-8213/ab2988 | arxiv=1906.10703 |issn=0004-637X|bibcode=2019ApJ...880L..17N|hdl=1721.1/124722|s2cid=195658207|hdl-access=free |doi-access=free }}</ref><ref name="Benatti et al.">{{Cite journal|last1=Benatti|first1=S.|last2=Nardiello|first2=D.|last3=Malavolta|first3=L.|last4=Desidera|first4=S.|last5=Borsato|first5=L.|last6=Nascimbeni|first6=V.|last7=Damasso|first7=M.|last8=D'Orazi|first8=V.|last9=Mesa|first9=D.|last10=Messina|first10=S.|last11=Esposito|first11=M.|last12=Bignamini|first12=A.|last13=Claudi|first13=R.|last14=Covino|first14=E.|last15=Lovis|first15=C.|last16=Sabotta|first16=S.|date=October 2019|title=A possibly inflated planet around the bright young star DS Tucanae A|journal= Astronomy & Astrophysics|language=en|volume=630|pages=A81|doi=10.1051/0004-6361/201935598|issn=0004-6361|bibcode=2019A&A...630A..81B|arxiv=1904.01591|s2cid=102486551}}</ref><ref>{{Cite web|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=DS+Tuc+A+b&type=CONFIRMED_PLANET|title=DS Tuc A b|website=exoplanetarchive.ipac.caltech.edu|access-date=2019-12-18}}</ref>


== Stellar system ==
== Stellar system ==
Line 97: Line 97:
DS Tuc Ab is one of the few [[Transit (astronomy)|transiting]] planets with an age smaller than 100 Myrs. Other examples are [[K2-33b]], [[V1298 Tauri|V1298 Tauri b]] and [[AU Microscopii b]]. Of these systems DS Tuc is the brightest and it is a good target for atmospheric characterization with [[James Webb Space Telescope|JWST]]. The planet is a [[super-Neptune]] or sub-Saturn.<ref name="Newton et al." /> The planet might be an inflated planet with an upper mass limit of 20 {{Earth mass|link=true}}.<ref name="Benatti et al." /> DS Tuc Ab will be observed by [[European Space Agency|ESA]]'s [[CHEOPS]] mission to characterize the planet.<ref>{{Cite web|url=https://www.cosmos.esa.int/web/cheops-guest-observers-programme/ao-1-programmes|title=AO-1 Programmes - CHEOPS Guest Observers Programme - Cosmos|website=www.cosmos.esa.int|access-date=2019-12-18}}</ref>
DS Tuc Ab is one of the few [[Transit (astronomy)|transiting]] planets with an age smaller than 100 Myrs. Other examples are [[K2-33b]], [[V1298 Tauri|V1298 Tauri b]] and [[AU Microscopii b]]. Of these systems DS Tuc is the brightest and it is a good target for atmospheric characterization with [[James Webb Space Telescope|JWST]]. The planet is a [[super-Neptune]] or sub-Saturn.<ref name="Newton et al." /> The planet might be an inflated planet with an upper mass limit of 20 {{Earth mass|link=true}}.<ref name="Benatti et al." /> DS Tuc Ab will be observed by [[European Space Agency|ESA]]'s [[CHEOPS]] mission to characterize the planet.<ref>{{Cite web|url=https://www.cosmos.esa.int/web/cheops-guest-observers-programme/ao-1-programmes|title=AO-1 Programmes - CHEOPS Guest Observers Programme - Cosmos|website=www.cosmos.esa.int|access-date=2019-12-18}}</ref>


The planet [[DS Tucanae Ab]] has a low orbital [[Axial tilt|obliquity]] (λ = {{Val|2.93|0.88|0.87|ul=°}} or λ = {{val|12|13|u=°}}). This means that the orbital plane of this planet aligns with the stellar equator of the star. This is unusual for a short period planet. Many short period planets show high orbital obliquity, which was taken as a sign of the scattering of the planet into this short period orbit. It can also be interpreted as the formation of a planet in an inner disk with an axial tilt. But these previous measurements of orbital obliquity were made for giant planets around mature stars. DS Tucanae Ab is a relatively small young planet. This suggests that DS Tucanae Ab formed in a smooth disk that was not perturbed by the stellar companion DS Tucanae B.<ref>{{cite journal|last1=Montet|first1=Benjamin T.|last2=Feinstein|first2=Adina D.|last3=Luger|first3=Rodrigo|last4=Bedell|first4=Megan E.|last5=Gully-Santiago|first5=Michael A.|last6=Teske|first6=Johanna K.|last7=Xuesong Wang|first7=Sharon|last8=Butler|first8=R. Paul|last9=Flowers|first9=Erin|last10=Shectman|first10=Stephen A.|last11=Crane|first11=Jeffrey D.|title=The Young Planet DS Tuc Ab has a Low Obliquity|journal=The Astronomical Journal|language=en|volume=159|issue=3|pages=112|arxiv=1912.03794|doi=10.3847/1538-3881/ab6d6d|bibcode=2020AJ....159..112M|year=2020|s2cid=208920990}}</ref><ref>{{cite journal|last1=Zhou|first1=G.|last2=Winn|first2=J. N.|last3=Newton|first3=E. R.|last4=Quinn|first4=S. N.|last5=Rodriguez|first5=J. E.|last6=Mann|first6=A. W.|last7=Rizzuto|first7=A. C.|last8=Vanderburg|first8=A. M.|last9=Huang|first9=C. X.|last10=Latham|first10=D. W.|last11=Teske|first11=J. K.|title=A well aligned orbit for the 45 Myr old transiting Neptune DS Tuc Ab|journal=The Astrophysical Journal|year=2020|language=en|volume=892|issue=2|pages=L21|doi=10.3847/2041-8213/ab7d3c|arxiv=1912.04095|bibcode=2020ApJ...892L..21Z|s2cid=208910672}}</ref> DS Tucanae Ab might therefore be a good target to study [[In situ#Astronomy|in-situ]] planet-formation of short-period planets.
The planet [[DS Tucanae Ab]] has a low orbital [[Axial tilt|obliquity]] (λ = {{Val|2.93|0.88|0.87|ul=°}} or λ = {{val|12|13|u=°}}). This means that the orbital plane of this planet aligns with the stellar equator of the star. This is unusual for a short period planet. Many short period planets show high orbital obliquity, which was taken as a sign of the scattering of the planet into this short period orbit. It can also be interpreted as the formation of a planet in an inner disk with an axial tilt. But these previous measurements of orbital obliquity were made for giant planets around mature stars. DS Tucanae Ab is a relatively small young planet. This suggests that DS Tucanae Ab formed in a smooth disk that was not perturbed by the stellar companion DS Tucanae B.<ref>{{cite journal|last1=Montet|first1=Benjamin T.|last2=Feinstein|first2=Adina D.|last3=Luger|first3=Rodrigo|last4=Bedell|first4=Megan E.|last5=Gully-Santiago|first5=Michael A.|last6=Teske|first6=Johanna K.|last7=Xuesong Wang|first7=Sharon|last8=Butler|first8=R. Paul|last9=Flowers|first9=Erin|last10=Shectman|first10=Stephen A.|last11=Crane|first11=Jeffrey D.|title=The Young Planet DS Tuc Ab has a Low Obliquity|journal=The Astronomical Journal|language=en|volume=159|issue=3|pages=112|arxiv=1912.03794|doi=10.3847/1538-3881/ab6d6d|bibcode=2020AJ....159..112M|year=2020|s2cid=208920990 |doi-access=free }}</ref><ref>{{cite journal|last1=Zhou|first1=G.|last2=Winn|first2=J. N.|last3=Newton|first3=E. R.|last4=Quinn|first4=S. N.|last5=Rodriguez|first5=J. E.|last6=Mann|first6=A. W.|last7=Rizzuto|first7=A. C.|last8=Vanderburg|first8=A. M.|last9=Huang|first9=C. X.|last10=Latham|first10=D. W.|last11=Teske|first11=J. K.|title=A well aligned orbit for the 45 Myr old transiting Neptune DS Tuc Ab|journal=The Astrophysical Journal|year=2020|language=en|volume=892|issue=2|pages=L21|doi=10.3847/2041-8213/ab7d3c|arxiv=1912.04095|bibcode=2020ApJ...892L..21Z|s2cid=208910672 |doi-access=free }}</ref> DS Tucanae Ab might therefore be a good target to study [[In situ#Astronomy|in-situ]] planet-formation of short-period planets.


== References ==
== References ==
Line 109: Line 109:


{{DEFAULTSORT:DS Tucanae}}
{{DEFAULTSORT:DS Tucanae}}
[[Category:Tucana (constellation)]]
[[Category:Tucana]]
[[Category:Henry Draper Catalogue objects|222259]]
[[Category:Henry Draper Catalogue objects|222259]]
[[Category:Hipparcos objects|116748]]
[[Category:Hipparcos objects|116748]]

Revision as of 06:18, 22 June 2024

DS Tucanae

DS Tucanae imaged with the NTT. DS Tucanae A is on the right and DS Tucanae B is on the left.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Tucana
DS Tucanae A
Right ascension 23h 39m 39.48081s[1]
Declination −69° 11′ 44.7077″[1]
Apparent magnitude (V) 8.47[2]
DS Tucanae B
Right ascension 23h 39m 39.26965s[3]
Declination −69° 11′ 39.4936″[3]
Apparent magnitude (V) 9.84[4]
Characteristics
Spectral type G6V+K3V[4]
Variable type RS CVn[5]
Astrometry
A
Radial velocity (Rv)7.20[6] km/s
Proper motion (μ) RA: 79.529[1] mas/yr
Dec.: −67.551[1] mas/yr
Parallax (π)22.6367 ± 0.0150 mas[1]
Distance144.08 ± 0.10 ly
(44.18 ± 0.03 pc)
B
Radial velocity (Rv)5.32[7] km/s
Proper motion (μ) RA: 78.133[3] mas/yr
Dec.: −65.845[3] mas/yr
Parallax (π)22.6524 ± 0.0125 mas[3]
Distance143.98 ± 0.08 ly
(44.15 ± 0.02 pc)
Details
DS Tucanae A
Mass1.01±0.06[8] M☉
Radius0.964±0.029[8] R☉
Luminosity0.725±0.013[8] L☉
Temperature5,428±80[8] K
Rotational velocity (v sin i)27.75+1.73
−1.54[9] km/s
Age45±4[8] Myr
DS Tucanae B
Mass0.84±0.06[8] M☉
Radius0.864±0.036[8] R☉
Luminosity0.327±0.010[8] L☉
Temperature4,700±90[8] K
Age45±4[8] Myr
Other designations
DS Tuc, HD 222259, CCDM J23397-6912AB, CD−69°2106, HIP 116748, WDS J23397-6912AB, TIC 410214986, TOI 200
Database references
SIMBADAB
A
B
Ab

DS Tucanae (HD 222259) is a binary star system 144 light years away in the constellation of Tucana. It has an apparent visual magnitude of 8.5,[8] and is a RS Canum Venaticorum variable.[5] The system is notable for being young as a member of the 45 Myr old Tucana-Horologium moving group[10] and for the primary star hosting the confirmed exoplanet DS Tucanae Ab, discovered by THYME, using TESS.[11][8][12][13]

Stellar system

A light curve for DS Tucanae, plotted from TESS data[14]

DS Tucanae is a visual binary.[4] The binary consists of a G6V primary and a K3V secondary separated by 5″.[15] Based on radial velocity measurements it was suggested that the secondary itself is a binary, but later studies could not find evidence for this claim.[8]

Physical properties

High levels of magnetic activity, a strong 6708Å lithium line, and the position on the color-magnitude diagram, slightly above the main sequence, strongly support a young age of the system.[12] The primary star is emitting a frequent and powerful (up to 5-8×1034 ergs) X-ray flares.[16]

Both components of the binary are main sequence stars. The primary has a mass very similar to the Sun, but slightly cooler and smaller, meaning it is only 72% as luminous as the Sun. The secondary is only 84% as massive as the Sun and only 33% as luminous.

Planetary system

The DS Tuc A planetary system[8][12]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b <14.4[9] M🜨 0.18+0.13
−0.12 		8.138268 — 88.73+0.18
−0.17[9]° 		5.70±0.17 R🜨

DS Tuc Ab is one of the few transiting planets with an age smaller than 100 Myrs. Other examples are K2-33b, V1298 Tauri b and AU Microscopii b. Of these systems DS Tuc is the brightest and it is a good target for atmospheric characterization with JWST. The planet is a super-Neptune or sub-Saturn.[8] The planet might be an inflated planet with an upper mass limit of 20 ME.[12] DS Tuc Ab will be observed by ESA's CHEOPS mission to characterize the planet.[17]

The planet DS Tucanae Ab has a low orbital obliquity (λ = 2.93°+0.88°
−0.87° or λ = 12°±13°). This means that the orbital plane of this planet aligns with the stellar equator of the star. This is unusual for a short period planet. Many short period planets show high orbital obliquity, which was taken as a sign of the scattering of the planet into this short period orbit. It can also be interpreted as the formation of a planet in an inner disk with an axial tilt. But these previous measurements of orbital obliquity were made for giant planets around mature stars. DS Tucanae Ab is a relatively small young planet. This suggests that DS Tucanae Ab formed in a smooth disk that was not perturbed by the stellar companion DS Tucanae B.[18][19] DS Tucanae Ab might therefore be a good target to study in-situ planet-formation of short-period planets.

References

  1. ^ a b c d e 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.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
  3. ^ a b c d e 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.
  4. ^ a b c Torres, G. (August 1988). "Visual Measurements of Southern Double Stars - Part Three". Astrophysics and Space Science. 147 (2): 257–266. Bibcode:1988Ap&SS.147..257T. doi:10.1007/BF00645670. ISSN 0004-640X. S2CID 116982206.
  5. ^ a b Samus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (July 2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates". Astronomy Letters. 29 (7): 468–479. Bibcode:2003AstL...29..468S. doi:10.1134/1.1589864. ISSN 1063-7737. S2CID 16299532.
  6. ^ 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.
  7. ^ 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.
  8. ^ a b c d e f g h i j k l m n o Newton, Elisabeth R.; et al. (July 2019). "TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana-Horologium Association". The Astrophysical Journal Letters. 880 (1): L17. arXiv:1906.10703. Bibcode:2019ApJ...880L..17N. doi:10.3847/2041-8213/ab2988. hdl:1721.1/124722. ISSN 0004-637X. S2CID 195658207.
  9. ^ a b c Benatti, S.; Damasso, M.; Borsa, F.; Locci, D.; Pillitteri, I.; Desidera, S.; Maggio, A.; Micela, G.; Wolk, S.; Claudi, R.; Malavolta, L.; Modirrousta-Galian, D. (2021), "Constraints on the mass and on the atmospheric composition and evolution of the low-density young planet DS Tucanae a B", Astronomy & Astrophysics, 650: A66, arXiv:2103.12922, Bibcode:2021A&A...650A..66B, doi:10.1051/0004-6361/202140416, S2CID 234864890
  10. ^ Zuckerman, B.; Webb, R. A. (2000-06-01). "Identification of a Nearby Stellar Association in theHipparcos Catalog: Implications for Recent, Local Star Formation". The Astrophysical Journal. 535 (2): 959. arXiv:astro-ph/0002461. Bibcode:2000ApJ...535..959Z. doi:10.1086/308897. ISSN 0004-637X. S2CID 2485534.
  11. ^ Albright, Charlotte (14 August 2019). "Dartmouth Astronomer on Leading Discovery of a New Planet | Dartmouth News". news.dartmouth.edu. Retrieved 2022-01-30.
  12. ^ a b c d Benatti, S.; Nardiello, D.; Malavolta, L.; Desidera, S.; Borsato, L.; Nascimbeni, V.; Damasso, M.; D'Orazi, V.; Mesa, D.; Messina, S.; Esposito, M.; Bignamini, A.; Claudi, R.; Covino, E.; Lovis, C.; Sabotta, S. (October 2019). "A possibly inflated planet around the bright young star DS Tucanae A". Astronomy & Astrophysics. 630: A81. arXiv:1904.01591. Bibcode:2019A&A...630A..81B. doi:10.1051/0004-6361/201935598. ISSN 0004-6361. S2CID 102486551.
  13. ^ "DS Tuc A b". exoplanetarchive.ipac.caltech.edu. Retrieved 2019-12-18.
  14. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  15. ^ Torres, C. a. O.; Quast, G. R.; Silva, L. da; Reza, R. de la; Melo, C. H. F.; Sterzik, M. (2006-12-01). "Search for associations containing young stars (SACY) - I. Sample and searching method". Astronomy & Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. ISSN 0004-6361. S2CID 16080025.
  16. ^ Pillitteri, I.; Argiroffi, C.; Maggio, A.; Micela, G.; Benatti, S.; Reale, F.; Colombo, S.; Wolk, S. J. (2022), "X-ray flares of the young planet host Ds Tucanae A", Astronomy & Astrophysics, 666: A198, arXiv:2208.07415, Bibcode:2022A&A...666A.198P, doi:10.1051/0004-6361/202244268, S2CID 251589568
  17. ^ "AO-1 Programmes - CHEOPS Guest Observers Programme - Cosmos". www.cosmos.esa.int. Retrieved 2019-12-18.
  18. ^ Montet, Benjamin T.; Feinstein, Adina D.; Luger, Rodrigo; Bedell, Megan E.; Gully-Santiago, Michael A.; Teske, Johanna K.; Xuesong Wang, Sharon; Butler, R. Paul; Flowers, Erin; Shectman, Stephen A.; Crane, Jeffrey D. (2020). "The Young Planet DS Tuc Ab has a Low Obliquity". The Astronomical Journal. 159 (3): 112. arXiv:1912.03794. Bibcode:2020AJ....159..112M. doi:10.3847/1538-3881/ab6d6d. S2CID 208920990.
  19. ^ Zhou, G.; Winn, J. N.; Newton, E. R.; Quinn, S. N.; Rodriguez, J. E.; Mann, A. W.; Rizzuto, A. C.; Vanderburg, A. M.; Huang, C. X.; Latham, D. W.; Teske, J. K. (2020). "A well aligned orbit for the 45 Myr old transiting Neptune DS Tuc Ab". The Astrophysical Journal. 892 (2): L21. arXiv:1912.04095. Bibcode:2020ApJ...892L..21Z. doi:10.3847/2041-8213/ab7d3c. S2CID 208910672.
Retrieved from "https://en.wikipedia.org/w/index.php?title=DS_Tucanae&oldid=1230348169"