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{{Starbox detail
{{Starbox detail
| source= <!--[source url]-->
| source= <!--[source url]-->
| mass= {{val|1.095|0.049|0.047}}<ref name=Feinstein>{{cite journal|doi=10.3847/2041-8213/ac4745|title=V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau E|year=2022|last1=Feinstein|first1=Adina D.|last2=David|first2=Trevor J.|last3=Montet|first3=Benjamin T.|last4=Foreman-Mackey|first4=Daniel|last5=Livingston|first5=John H.|last6=Mann|first6=Andrew W.|journal=The Astrophysical Journal Letters|volume=925|issue=1|pages=L2|arxiv=2111.08660|bibcode=2022ApJ...925L...2F|s2cid=244130016}}</ref>
| mass= {{val|1.095|0.049|0.047}}<ref name=Feinstein>{{cite journal|doi=10.3847/2041-8213/ac4745|title=V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau E|year=2022|last1=Feinstein|first1=Adina D.|last2=David|first2=Trevor J.|last3=Montet|first3=Benjamin T.|last4=Foreman-Mackey|first4=Daniel|last5=Livingston|first5=John H.|last6=Mann|first6=Andrew W.|journal=The Astrophysical Journal Letters|volume=925|issue=1|pages=L2|arxiv=2111.08660|bibcode=2022ApJ...925L...2F|s2cid=244130016 |doi-access=free }}</ref>
| radius= {{val|1.33|0.04|0.03}}<ref name=Feinstein/>
| radius= {{val|1.33|0.04|0.03}}<ref name=Feinstein/>
| luminosity= 0.934 ± 0.044<ref name="David et al 1" />
| luminosity= 0.934 ± 0.044<ref name="David et al 1" />
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'''V1298 Tauri''' is a young (23±4 [[Myr]]) weakly-lined [[T Tauri star]]<ref name="David et al 2" /> that is part of the [[Taurus-Auriga association]] in the [[Taurus Molecular Cloud]]. Alternatively it is part of a proposed moving group, called [[Group 29 (stellar association)|Group 29]] that is slightly older.<ref name="Oh et al">{{Cite journal|last1=Oh|first1=Semyeong|last2=Price-Whelan|first2=Adrian M.|last3=Hogg|first3=David W.|last4=Morton|first4=Timothy D.|last5=Spergel|first5=David N.|date=June 2017|title=Comoving Stars in Gaia DR1: An Abundance of Very Wide Separation Comoving Pairs|journal=The Astronomical Journal|language=en|volume=153|issue=6|pages=257|doi=10.3847/1538-3881/aa6ffd|bibcode=2017AJ....153..257O|issn=0004-6256|arxiv=1612.02440|s2cid=119351439}}</ref><ref>{{Cite journal|last=Luhman|first=K. L.|date=December 2018|title=The Stellar Membership of the Taurus Star-forming Region|journal=The Astronomical Journal|language=en|volume=156|issue=6|pages=271|doi=10.3847/1538-3881/aae831|arxiv=1811.01359|bibcode=2018AJ....156..271L|s2cid=119471553|issn=0004-6256}}</ref><ref name="David et al 1">{{Cite journal|last1=David|first1=Trevor J.|last2=Cody|first2=Ann Marie|last3=Hedges|first3=Christina L.|last4=Mamajek|first4=Eric E.|last5=Hillenbrand|first5=Lynne A.|last6=Ciardi|first6=David R.|last7=Beichman|first7=Charles A.|last8=Petigura|first8=Erik A.|last9=Fulton|first9=Benjamin J.|last10=Isaacson|first10=Howard T.|last11=Howard|first11=Andrew W.|date=August 2019|title=A Warm Jupiter-sized Planet Transiting the Pre-main-sequence Star V1298 Tau|journal=The Astronomical Journal|language=en|volume=158|issue=2|pages=79|doi=10.3847/1538-3881/ab290f|arxiv=1902.09670|bibcode=2019AJ....158...79D|s2cid=119003936|issn=0004-6256}}</ref> The system has four transiting [[exoplanet]]s, discovered with the [[Kepler space telescope]] in the K2 mission.<ref name="David et al 2" /> One of the planets was discovered in August 2019<ref name="David et al 1" /> and the other three were discovered in November 2019 by the same team.<ref name="David et al 2" />
'''V1298 Tauri''' is a young (23±4 [[Myr]]) weakly-lined [[T Tauri star]]<ref name="David et al 2" /> that is part of the [[Taurus-Auriga association]] in the [[Taurus Molecular Cloud]]. Alternatively it is part of a proposed moving group, called [[Group 29 (stellar association)|Group 29]] that is slightly older.<ref name="Oh et al">{{Cite journal|last1=Oh|first1=Semyeong|last2=Price-Whelan|first2=Adrian M.|last3=Hogg|first3=David W.|last4=Morton|first4=Timothy D.|last5=Spergel|first5=David N.|date=June 2017|title=Comoving Stars in Gaia DR1: An Abundance of Very Wide Separation Comoving Pairs|journal=The Astronomical Journal|language=en|volume=153|issue=6|pages=257|doi=10.3847/1538-3881/aa6ffd|bibcode=2017AJ....153..257O|issn=0004-6256|arxiv=1612.02440|s2cid=119351439 |doi-access=free }}</ref><ref>{{Cite journal|last=Luhman|first=K. L.|date=December 2018|title=The Stellar Membership of the Taurus Star-forming Region|journal=The Astronomical Journal|language=en|volume=156|issue=6|pages=271|doi=10.3847/1538-3881/aae831|arxiv=1811.01359|bibcode=2018AJ....156..271L|s2cid=119471553|issn=0004-6256 |doi-access=free }}</ref><ref name="David et al 1">{{Cite journal|last1=David|first1=Trevor J.|last2=Cody|first2=Ann Marie|last3=Hedges|first3=Christina L.|last4=Mamajek|first4=Eric E.|last5=Hillenbrand|first5=Lynne A.|last6=Ciardi|first6=David R.|last7=Beichman|first7=Charles A.|last8=Petigura|first8=Erik A.|last9=Fulton|first9=Benjamin J.|last10=Isaacson|first10=Howard T.|last11=Howard|first11=Andrew W.|date=August 2019|title=A Warm Jupiter-sized Planet Transiting the Pre-main-sequence Star V1298 Tau|journal=The Astronomical Journal|language=en|volume=158|issue=2|pages=79|doi=10.3847/1538-3881/ab290f|arxiv=1902.09670|bibcode=2019AJ....158...79D|s2cid=119003936|issn=0004-6256 |doi-access=free }}</ref> The system has four transiting [[exoplanet]]s, discovered with the [[Kepler space telescope]] in the K2 mission.<ref name="David et al 2" /> One of the planets was discovered in August 2019<ref name="David et al 1" /> and the other three were discovered in November 2019 by the same team.<ref name="David et al 2" />


== Stellar characteristics ==
== Stellar characteristics ==
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V1298 Tauri has four confirmed planets of which planets c, d and b are near a 1:2:3 [[Orbital resonance|resonance]] (with periods of 8.25, 12.40 and 24.14 days). Planet e only shows a single transit in the K2 light curve and has a period larger than 36 days. Planet e might be in a low-order resonance (of 2:3, 3:5, 1:2, or 1:3) with planet b. The system is very young and might be a precursor of a compact multiplanet system. The 2:3 resonance suggests that some close-in planets may either form in resonances or evolve into them on timescales of less than 10 Myr. The planets in the system have a size between Neptune and Saturn. Only planet b has a size similar to Jupiter.<ref name="David et al 2" />
V1298 Tauri has four confirmed planets of which planets c, d and b are near a 1:2:3 [[Orbital resonance|resonance]] (with periods of 8.25, 12.40 and 24.14 days). Planet e only shows a single transit in the K2 light curve and has a period larger than 36 days. Planet e might be in a low-order resonance (of 2:3, 3:5, 1:2, or 1:3) with planet b. The system is very young and might be a precursor of a compact multiplanet system. The 2:3 resonance suggests that some close-in planets may either form in resonances or evolve into them on timescales of less than 10 Myr. The planets in the system have a size between Neptune and Saturn. Only planet b has a size similar to Jupiter.<ref name="David et al 2" />


Models predict that the planets have a minimum core mass of 5 {{Earth mass|link=true}} and are surrounded by a thick envelope that make up 20% of their mass. The total mass of planet c and d was predicted to be 2 - 28 {{Earth mass}} and the total mass of planet d and b was predicted to be 9 - 120 {{Earth mass}}.<ref name="David et al 2">{{Cite journal|last1=David|first1=Trevor J.|last2=Petigura|first2=Erik A.|last3=Luger|first3=Rodrigo|last4=Foreman-Mackey|first4=Daniel|last5=Livingston|first5=John H.|last6=Mamajek|first6=Eric E.|last7=Hillenbrand|first7=Lynne A.|date=2019-10-29|title=Four Newborn Planets Transiting the Young Solar Analog V1298 Tau|journal=The Astrophysical Journal|volume=885|issue=1|pages=L12|arxiv=1910.04563|bibcode=2019ApJ...885L..12D|doi=10.3847/2041-8213/ab4c99|s2cid=204008446|issn=2041-8213}}</ref> In a follow-up paper the mass of [[V1298 Tauri b]] was constrained to <2.2 {{Jupiter mass|link=true}}.<ref name="Beichman et al">{{Cite journal|last1=Beichman|first1=Charles|last2=Hirano|first2=Teruyuki|last3=David|first3=Trevor J.|last4=Kotani|first4=Takayuki|last5=Hillenbrand|first5=Lynne A.|last6=Vasisht|first6=Gautam|last7=Ciardi|first7=David R.|last8=Harakawa|first8=Hiroki|last9=Kudo|first9=Tomoyuki|last10=Omiya|first10=Masashi|last11=Kuzuhara|first11=Masayuki|date=June 2019|title=A Mass Limit for the Young Transiting Planet V1298 Tau b|journal=Research Notes of the AAS|language=en|volume=3|issue=6|pages=89|doi=10.3847/2515-5172/ab2c9d|bibcode=2019RNAAS...3...89B|issn=2515-5172}}</ref> The planet c was suspected to be shedding mass due to intense irradiation by the host star, but hydrogen tail existence was refuted by 2021.<ref>{{citation|arxiv=2108.08851|year=2021|title=H-Alpha Variability of V1298 Tau c}}</ref>
Models predict that the planets have a minimum core mass of 5 {{Earth mass|link=true}} and are surrounded by a thick envelope that make up 20% of their mass. The total mass of planet c and d was predicted to be 2 - 28 {{Earth mass}} and the total mass of planet d and b was predicted to be 9 - 120 {{Earth mass}}.<ref name="David et al 2">{{Cite journal|last1=David|first1=Trevor J.|last2=Petigura|first2=Erik A.|last3=Luger|first3=Rodrigo|last4=Foreman-Mackey|first4=Daniel|last5=Livingston|first5=John H.|last6=Mamajek|first6=Eric E.|last7=Hillenbrand|first7=Lynne A.|date=2019-10-29|title=Four Newborn Planets Transiting the Young Solar Analog V1298 Tau|journal=The Astrophysical Journal|volume=885|issue=1|pages=L12|arxiv=1910.04563|bibcode=2019ApJ...885L..12D|doi=10.3847/2041-8213/ab4c99|s2cid=204008446|issn=2041-8213 |doi-access=free }}</ref> In a follow-up paper the mass of [[V1298 Tauri b]] was constrained to <2.2 {{Jupiter mass|link=true}}.<ref name="Beichman et al">{{Cite journal|last1=Beichman|first1=Charles|last2=Hirano|first2=Teruyuki|last3=David|first3=Trevor J.|last4=Kotani|first4=Takayuki|last5=Hillenbrand|first5=Lynne A.|last6=Vasisht|first6=Gautam|last7=Ciardi|first7=David R.|last8=Harakawa|first8=Hiroki|last9=Kudo|first9=Tomoyuki|last10=Omiya|first10=Masashi|last11=Kuzuhara|first11=Masayuki|date=June 2019|title=A Mass Limit for the Young Transiting Planet V1298 Tau b|journal=Research Notes of the AAS|language=en|volume=3|issue=6|pages=89|doi=10.3847/2515-5172/ab2c9d|bibcode=2019RNAAS...3...89B|s2cid=198445373 |issn=2515-5172|doi-access=free}}</ref> The planet c was suspected to be shedding mass due to intense irradiation by the host star, but hydrogen tail existence was refuted by 2021.<ref>{{citation|arxiv=2108.08851|year=2021|title=H-Alpha Variability of V1298 Tau c|last1=Schlawin |first1=Everett |last2=Ilyin |first2=Ilya |last3=Feinstein |first3=Adina D. |last4=Bean |first4=Jacob |last5=Huang |first5=Chenliang |last6=Gao |first6=Peter |last7=Strassmeier |first7=Klaus |last8=Poppenhaeger |first8=Katja |journal=Research Notes of the American Astronomical Society |volume=5 |issue=8 |page=195 |doi=10.3847/2515-5172/ac1f2f |bibcode=2021RNAAS...5..195S |s2cid=237250293 |doi-access=free }}</ref>


Orbits of the planets b and c are nearly coplanar and planet c is not inclined to the equatorial plane of the star, misalignment equals to 2{{±|12|4}} degrees.<ref>{{citation|arxiv=2110.10689|year=2021|title=Zodiacal Exoplanets in Time (ZEIT) XIII: Planet Orbits and Atmospheres in the V1298 Tau System, a Keystone in Studies of Early Planetary Evolution}}</ref>
Orbits of the planets b and c are nearly coplanar and planet c is not inclined to the equatorial plane of the star, misalignment equals to 2{{±|12|4}} degrees.<ref>{{citation|arxiv=2110.10689|year=2022|title=Zodiacal exoplanets in time – XIII. Planet orbits and atmospheres in the V1298 Tau system, a keystone in studies of early planetary evolution|doi=10.1093/mnras/stab3107 |last1=Gaidos |first1=E. |last2=Hirano |first2=T. |last3=Beichman |first3=C. |last4=Livingston |first4=J. |last5=Harakawa |first5=H. |last6=Hodapp |first6=K. W. |last7=Ishizuka |first7=M. |last8=Jacobson |first8=S. |last9=Konishi |first9=M. |last10=Kotani |first10=T. |last11=Kudo |first11=T. |last12=Kurokawa |first12=T. |last13=Kuzuhara |first13=M. |last14=Nishikawa |first14=J. |last15=Omiya |first15=M. |last16=Serizawa |first16=T. |last17=Tamura |first17=M. |last18=Ueda |first18=A. |last19=Vievard |first19=S. |journal=Monthly Notices of the Royal Astronomical Society |volume=509 |issue=2 |pages=2969–2978 }}</ref>


{{OrbitboxPlanet begin
{{OrbitboxPlanet begin
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}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
|exoplanet= [[V1298 Tauri c|c]]
|exoplanet= c
|mass=
|mass=
|period= 8.24958 ± 0.00072
|period= 8.24958 ± 0.00072
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}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
|exoplanet= [[V1298 Tauri d|d]]
|exoplanet= d
|mass=
|mass=
|period= 12.4032 ± 0.0015
|period= 12.4032 ± 0.0015
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}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
|exoplanet= [[V1298 Tauri b|b]]
|exoplanet= b
|mass= <2.2
|mass= <2.2
|period= 24.1396 ± 0.0018
|period= 24.1396 ± 0.0018
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}}
}}
{{OrbitboxPlanet
{{OrbitboxPlanet
|exoplanet= [[V1298 Tauri e|e]]
|exoplanet= e
|mass=
|mass=
|period= 50.29{{±|6.62}}<ref name=Feinstein2021>{{citation|arxiv=2111.08660|year=2021|title=V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau e}}</ref>
|period= 50.29{{±|6.62}}<ref name=Feinstein2021>{{citation|arxiv=2111.08660|year=2022|title=V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau E|doi=10.3847/2041-8213/ac4745 |last1=Feinstein |first1=Adina D. |last2=David |first2=Trevor J. |last3=Montet |first3=Benjamin T. |last4=Foreman-Mackey |first4=Daniel |last5=Livingston |first5=John H. |last6=Mann |first6=Andrew W. |journal=The Astrophysical Journal Letters |volume=925 |issue=1 |pages=L2 |bibcode=2022ApJ...925L...2F |s2cid=244130016 |doi-access=free }}</ref>
|semimajor= {{val|0.308|0.182|0.066}}
|semimajor= {{val|0.308|0.182|0.066}}
|radius= 0.89{{±|0.04}}<ref name=Feinstein2021/>
|radius= 0.89{{±|0.04}}<ref name=Feinstein2021/>

Revision as of 16:51, 4 March 2024

V1298 Tauri

The planetary system V1298 Tauri
Credit: Exoplanet Exploration Program and the Jet Propulsion Laboratory for NASA’s Astrophysics Division
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Taurus
Right ascension 04h 05m 19.59121s[1]
Declination +20° 09′ 25.5635″[1]
Apparent magnitude (V) 10.31 - 10.43[2]
Characteristics
Spectral type K0-K1.5[3]
Variable type Irregular[2]
Astrometry
Proper motion (μ) RA: 5.228 ± 0.131[1] mas/yr
Dec.: -16.077 ± 0.048[1] mas/yr
Parallax (π)9.2139 ± 0.0593 mas[1]
Distance354 ± 2 ly
(108.5 ± 0.7 pc)
Details
Mass1.095+0.049
−0.047[4] M☉
Radius1.33+0.04
−0.03[4] R☉
Luminosity0.934 ± 0.044[3] L☉
Temperature4970 ± 120[3] K
Rotation2.97+0.03
−0.04 d[4]
Age23 ± 4[3] Myr
Other designations
K2-309, 2MASS J04051959+2009256, BD+19 656, EPIC 210818897, RX J0405.3+2009, 1SWASP J040519.59+200925.5
Database references
SIMBADdata

V1298 Tauri is a young (23±4 Myr) weakly-lined T Tauri star[5] that is part of the Taurus-Auriga association in the Taurus Molecular Cloud. Alternatively it is part of a proposed moving group, called Group 29 that is slightly older.[6][7][3] The system has four transiting exoplanets, discovered with the Kepler space telescope in the K2 mission.[5] One of the planets was discovered in August 2019[3] and the other three were discovered in November 2019 by the same team.[5]

Stellar characteristics

A light curve for V1298 Tauri, adapted from David et al. (2019)[3]

V1298 Tauri has a spectral type of K0 - K1.5 and it has a mass of about 1.1 M☉. The star appears in x-rays from ROSAT data and it does show strong lithium absorption lines, both signatures of youth and therefore it was a proposed member of Taurus-Auriga. On the other hand it does not show signs of accretion and it lacks infrared excess. Instead it shows H-alpha in absorption.[3]

The brightness of V1298 Tauri varies in an unpredictable way between a maximum visual magnitude of 10.31 and a minimum of 10.54.[2] The light curve of the star shows quasi-periodic variability that was interpreted as stellar rotation and starspots. The light curve also showed several flares.[3]

Based on Gaia DR2 data this star is part of a co-moving pair, together with HD 284154.[6]

Planetary system

V1298 Tauri has four confirmed planets of which planets c, d and b are near a 1:2:3 resonance (with periods of 8.25, 12.40 and 24.14 days). Planet e only shows a single transit in the K2 light curve and has a period larger than 36 days. Planet e might be in a low-order resonance (of 2:3, 3:5, 1:2, or 1:3) with planet b. The system is very young and might be a precursor of a compact multiplanet system. The 2:3 resonance suggests that some close-in planets may either form in resonances or evolve into them on timescales of less than 10 Myr. The planets in the system have a size between Neptune and Saturn. Only planet b has a size similar to Jupiter.[5]

Models predict that the planets have a minimum core mass of 5 ME and are surrounded by a thick envelope that make up 20% of their mass. The total mass of planet c and d was predicted to be 2 - 28 ME and the total mass of planet d and b was predicted to be 9 - 120 ME.[5] In a follow-up paper the mass of V1298 Tauri b was constrained to <2.2 MJ.[8] The planet c was suspected to be shedding mass due to intense irradiation by the host star, but hydrogen tail existence was refuted by 2021.[9]

Orbits of the planets b and c are nearly coplanar and planet c is not inclined to the equatorial plane of the star, misalignment equals to 2+12
−4 degrees.[10]

The V 1298 Tauri planetary system[5][8]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c — 0.0825 ± 0.0013 8.24958 ± 0.00072 <0.43 88.49+0.92
−0.72° 		0.499+0.032
−0.029 RJ
d — 0.1083 ± 0.0017 12.4032 ± 0.0015 <0.21 89.04+0.65
−0.73° 		0.572+0.040
−0.035 RJ
b <2.2 MJ 0.1688 ± 0.0026 24.1396 ± 0.0018 <0.29 89.00+0.46
−0.24° 		0.916+0.052
−0.047 RJ
e — 0.308+0.182
−0.066 		50.29±6.62[11] <0.57 89.40+0.26
−0.18° 		0.89±0.04[11] RJ

See also

References

  1. ^ a b c d e Gaia Collaboration (2018-08-01). "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. ISSN 0004-6361. S2CID 49211658.
  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 c d e f g h i David, Trevor J.; Cody, Ann Marie; Hedges, Christina L.; Mamajek, Eric E.; Hillenbrand, Lynne A.; Ciardi, David R.; Beichman, Charles A.; Petigura, Erik A.; Fulton, Benjamin J.; Isaacson, Howard T.; Howard, Andrew W. (August 2019). "A Warm Jupiter-sized Planet Transiting the Pre-main-sequence Star V1298 Tau". The Astronomical Journal. 158 (2): 79. arXiv:1902.09670. Bibcode:2019AJ....158...79D. doi:10.3847/1538-3881/ab290f. ISSN 0004-6256. S2CID 119003936.
  4. ^ a b c Feinstein, Adina D.; David, Trevor J.; Montet, Benjamin T.; Foreman-Mackey, Daniel; Livingston, John H.; Mann, Andrew W. (2022). "V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau E". The Astrophysical Journal Letters. 925 (1): L2. arXiv:2111.08660. Bibcode:2022ApJ...925L...2F. doi:10.3847/2041-8213/ac4745. S2CID 244130016.
  5. ^ a b c d e f David, Trevor J.; Petigura, Erik A.; Luger, Rodrigo; Foreman-Mackey, Daniel; Livingston, John H.; Mamajek, Eric E.; Hillenbrand, Lynne A. (2019-10-29). "Four Newborn Planets Transiting the Young Solar Analog V1298 Tau". The Astrophysical Journal. 885 (1): L12. arXiv:1910.04563. Bibcode:2019ApJ...885L..12D. doi:10.3847/2041-8213/ab4c99. ISSN 2041-8213. S2CID 204008446.
  6. ^ a b Oh, Semyeong; Price-Whelan, Adrian M.; Hogg, David W.; Morton, Timothy D.; Spergel, David N. (June 2017). "Comoving Stars in Gaia DR1: An Abundance of Very Wide Separation Comoving Pairs". The Astronomical Journal. 153 (6): 257. arXiv:1612.02440. Bibcode:2017AJ....153..257O. doi:10.3847/1538-3881/aa6ffd. ISSN 0004-6256. S2CID 119351439.
  7. ^ Luhman, K. L. (December 2018). "The Stellar Membership of the Taurus Star-forming Region". The Astronomical Journal. 156 (6): 271. arXiv:1811.01359. Bibcode:2018AJ....156..271L. doi:10.3847/1538-3881/aae831. ISSN 0004-6256. S2CID 119471553.
  8. ^ a b Beichman, Charles; Hirano, Teruyuki; David, Trevor J.; Kotani, Takayuki; Hillenbrand, Lynne A.; Vasisht, Gautam; Ciardi, David R.; Harakawa, Hiroki; Kudo, Tomoyuki; Omiya, Masashi; Kuzuhara, Masayuki (June 2019). "A Mass Limit for the Young Transiting Planet V1298 Tau b". Research Notes of the AAS. 3 (6): 89. Bibcode:2019RNAAS...3...89B. doi:10.3847/2515-5172/ab2c9d. ISSN 2515-5172. S2CID 198445373.
  9. ^ Schlawin, Everett; Ilyin, Ilya; Feinstein, Adina D.; Bean, Jacob; Huang, Chenliang; Gao, Peter; Strassmeier, Klaus; Poppenhaeger, Katja (2021), "H-Alpha Variability of V1298 Tau c", Research Notes of the American Astronomical Society, 5 (8): 195, arXiv:2108.08851, Bibcode:2021RNAAS...5..195S, doi:10.3847/2515-5172/ac1f2f, S2CID 237250293
  10. ^ Gaidos, E.; Hirano, T.; Beichman, C.; Livingston, J.; Harakawa, H.; Hodapp, K. W.; Ishizuka, M.; Jacobson, S.; Konishi, M.; Kotani, T.; Kudo, T.; Kurokawa, T.; Kuzuhara, M.; Nishikawa, J.; Omiya, M.; Serizawa, T.; Tamura, M.; Ueda, A.; Vievard, S. (2022), "Zodiacal exoplanets in time – XIII. Planet orbits and atmospheres in the V1298 Tau system, a keystone in studies of early planetary evolution", Monthly Notices of the Royal Astronomical Society, 509 (2): 2969–2978, arXiv:2110.10689, doi:10.1093/mnras/stab3107{{citation}}: CS1 maint: unflagged free DOI (link)
  11. ^ a b Feinstein, Adina D.; David, Trevor J.; Montet, Benjamin T.; Foreman-Mackey, Daniel; Livingston, John H.; Mann, Andrew W. (2022), "V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau E", The Astrophysical Journal Letters, 925 (1): L2, arXiv:2111.08660, Bibcode:2022ApJ...925L...2F, doi:10.3847/2041-8213/ac4745, S2CID 244130016
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