Descubren un exoplaneta del tamaño de Júpiter con características ...
Este planeta fue denominado NGTS-30 b / TOI-4862 b y orbita a una estrella que se encuentra a 762 años luz de distancia. Fue descubierto gracias ...
detectaron un exoplaneta
En esta ocasión, un grupo de investigadores de la Universidad de Ginebra dirigidos por Matthew Battley <anchor>detectaron un exoplaneta</anchor> de tamaño y masa similares a Júpiter (0,93 radios de Júpiter y 0,96 masas de Júpiter). Este planeta fue denominado NGTS-30 b / TOI-4862 b y orbita a una estrella que se encuentra a 762 años luz de distancia. Fue descubierto gracias al Satélite de Sondeo de Exoplanetas en Tránsito (TESS, por sus siglas en inglés) de la NASA.
[2404.02974] NGTS-30 b/TOI-4862 b: An 1 Gyr old 98-day transiting warm Jupiter
\[2404.02974\] NGTS-30 b/TOI-4862 b: An 1 Gyr old 98-day transiting warm Jupiter

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# Astrophysics > Earth and Planetary Astrophysics

**arXiv:2404.02974** (astro-ph)


\[Submitted on 3 Apr 2024\]

# Title:NGTS-30 b/TOI-4862 b: An 1 Gyr old 98-day transiting warm Jupiter

Authors: [M.P. Battley](https://arxiv.org/search/astro-ph?searchtype=author&query=Battley,+M), [K.A. Collins](https://arxiv.org/search/astro-ph?searchtype=author&query=Collins,+K), [S. Ulmer-Moll](https://arxiv.org/search/astro-ph?searchtype=author&query=Ulmer-Moll,+S), [S.N. Quinn](https://arxiv.org/search/astro-ph?searchtype=author&query=Quinn,+S), [M. Lendl](https://arxiv.org/search/astro-ph?searchtype=author&query=Lendl,+M), [S. Gill](https://arxiv.org/search/astro-ph?searchtype=author&query=Gill,+S), [R. Brahm](https://arxiv.org/search/astro-ph?searchtype=author&query=Brahm,+R), [M.J. Hobson](https://arxiv.org/search/astro-ph?searchtype=author&query=Hobson,+M), [H.P. Osborn](https://arxiv.org/search/astro-ph?searchtype=author&query=Osborn,+H), [A. Deline](https://arxiv.org/search/astro-ph?searchtype=author&query=Deline,+A), [J.P. Faria](https://arxiv.org/search/astro-ph?searchtype=author&query=Faria,+J), [A.B. Claringbold](https://arxiv.org/search/astro-ph?searchtype=author&query=Claringbold,+A), [H. Chakraborty](https://arxiv.org/search/astro-ph?searchtype=author&query=Chakraborty,+H), [K.G. Stassun](https://arxiv.org/search/astro-ph?searchtype=author&query=Stassun,+K), [C. Hellier](https://arxiv.org/search/astro-ph?searchtype=author&query=Hellier,+C), [D.R. Alves](https://arxiv.org/search/astro-ph?searchtype=author&query=Alves,+D), [C. Ziegler](https://arxiv.org/search/astro-ph?searchtype=author&query=Ziegler,+C), [D.R. Anderson](https://arxiv.org/search/astro-ph?searchtype=author&query=Anderson,+D), [I. Apergis](https://arxiv.org/search/astro-ph?searchtype=author&query=Apergis,+I), [D.J. Armstrong](https://arxiv.org/search/astro-ph?searchtype=author&query=Armstrong,+D), [D. Bayliss](https://arxiv.org/search/astro-ph?searchtype=author&query=Bayliss,+D), [Y. Beletsky](https://arxiv.org/search/astro-ph?searchtype=author&query=Beletsky,+Y), [A. Bieryla](https://arxiv.org/search/astro-ph?searchtype=author&query=Bieryla,+A), [F. Bouchy](https://arxiv.org/search/astro-ph?searchtype=author&query=Bouchy,+F), [M.R. Burleigh](https://arxiv.org/search/astro-ph?searchtype=author&query=Burleigh,+M), [R.P. Butler](https://arxiv.org/search/astro-ph?searchtype=author&query=Butler,+R), [S.L. Casewell](https://arxiv.org/search/astro-ph?searchtype=author&query=Casewell,+S), [J.L. Christiansen](https://arxiv.org/search/astro-ph?searchtype=author&query=Christiansen,+J), [J.D. Crane](https://arxiv.org/search/astro-ph?searchtype=author&query=Crane,+J), [P.A. Dalba](https://arxiv.org/search/astro-ph?searchtype=author&query=Dalba,+P), [T. Daylan](https://arxiv.org/search/astro-ph?searchtype=author&query=Daylan,+T), [P. Figueira](https://arxiv.org/search/astro-ph?searchtype=author&query=Figueira,+P), [E. Gillen](https://arxiv.org/search/astro-ph?searchtype=author&query=Gillen,+E), [M.R. Goad](https://arxiv.org/search/astro-ph?searchtype=author&query=Goad,+M), [M.N. Günther](https://arxiv.org/search/astro-ph?searchtype=author&query=G%C3%BCnther,+M), [B.A. Henderson](https://arxiv.org/search/astro-ph?searchtype=author&query=Henderson,+B), [T. Henning](https://arxiv.org/search/astro-ph?searchtype=author&query=Henning,+T), [J.S. Jenkins](https://arxiv.org/search/astro-ph?searchtype=author&query=Jenkins,+J), [A. Jordán](https://arxiv.org/search/astro-ph?searchtype=author&query=Jord%C3%A1n,+A), [S. Kanodia](https://arxiv.org/search/astro-ph?searchtype=author&query=Kanodia,+S), [A. Kendall](https://arxiv.org/search/astro-ph?searchtype=author&query=Kendall,+A), [M. Kunimoto](https://arxiv.org/search/astro-ph?searchtype=author&query=Kunimoto,+M), [D.W. Latham](https://arxiv.org/search/astro-ph?searchtype=author&query=Latham,+D), [A.M. Levine](https://arxiv.org/search/astro-ph?searchtype=author&query=Levine,+A), [J. McCormac](https://arxiv.org/search/astro-ph?searchtype=author&query=McCormac,+J), [M. Moyano](https://arxiv.org/search/astro-ph?searchtype=author&query=Moyano,+M), [A. Osborn](https://arxiv.org/search/astro-ph?searchtype=author&query=Osborn,+A), [D. Osip](https://arxiv.org/search/astro-ph?searchtype=author&query=Osip,+D), [T.A. Pritchard](https://arxiv.org/search/astro-ph?searchtype=author&query=Pritchard,+T), [A. Psaridi](https://arxiv.org/search/astro-ph?searchtype=author&query=Psaridi,+A), [M. Rice](https://arxiv.org/search/astro-ph?searchtype=author&query=Rice,+M), [J.E. Rodriguez](https://arxiv.org/search/astro-ph?searchtype=author&query=Rodriguez,+J), [S. Saha](https://arxiv.org/search/astro-ph?searchtype=author&query=Saha,+S), [S. Seager](https://arxiv.org/search/astro-ph?searchtype=author&query=Seager,+S), [S.A. Shectman](https://arxiv.org/search/astro-ph?searchtype=author&query=Shectman,+S), [A.M.S. Smith](https://arxiv.org/search/astro-ph?searchtype=author&query=Smith,+A), [J.K. Teske](https://arxiv.org/search/astro-ph?searchtype=author&query=Teske,+J), [E.B. Ting](https://arxiv.org/search/astro-ph?searchtype=author&query=Ting,+E), [S. Udry](https://arxiv.org/search/astro-ph?searchtype=author&query=Udry,+S), [J.I. Vines](https://arxiv.org/search/astro-ph?searchtype=author&query=Vines,+J), [C.A. Watson](https://arxiv.org/search/astro-ph?searchtype=author&query=Watson,+C), [R.G. West](https://arxiv.org/search/astro-ph?searchtype=author&query=West,+R), [P.J. Wheatley](https://arxiv.org/search/astro-ph?searchtype=author&query=Wheatley,+P), [J.N. Winn](https://arxiv.org/search/astro-ph?searchtype=author&query=Winn,+J), [S.W. Yee](https://arxiv.org/search/astro-ph?searchtype=author&query=Yee,+S), [Y. Zhao](https://arxiv.org/search/astro-ph?searchtype=author&query=Zhao,+Y)

View a PDF of the paper titled NGTS-30 b/TOI-4862 b: An 1 Gyr old 98-day transiting warm Jupiter, by M.P. Battley and 65 other authors

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> Abstract:Long-period transiting exoplanets bridge the gap between the bulk of transit- and Doppler-based exoplanet discoveries, providing key insights into the formation and evolution of planetary systems. The wider separation between these planets and their host stars results in the exoplanets typically experiencing less radiation from their host stars; hence, they should maintain more of their original atmospheres, which can be probed during transit via transmission spectroscopy. Although the known population of long-period transiting exoplanets is relatively sparse, surveys performed by the Transiting Exoplanet Survey Satellite (TESS) and the Next Generation Transit Survey (NGTS) are now discovering new exoplanets to fill in this crucial region of the exoplanetary parameter space. This study presents the detection and characterisation of NGTS-30 b/TOI-4862 b, a new long-period transiting exoplanet detected by following up on a single-transit candidate found in the TESS mission. Through monitoring using a combination of photometric instruments (TESS, NGTS, and EulerCam) and spectroscopic instruments (CORALIE, FEROS, HARPS, and PFS), NGTS-30 b/TOI-4862 b was found to be a long-period (P = 98.29838 day) Jupiter-sized (0.928 RJ; 0.960 MJ) planet transiting a 1.1 Gyr old G-type star. With a moderate eccentricity of 0.294, its equilibrium temperature could be expected to vary from 274 K to 500 K over the course of its orbit. Through interior modelling, NGTS-30 b/TOI-4862 b was found to have a heavy element mass fraction of 0.23 and a heavy element enrichment (Zp/Z\_star) of 20, making it metal-enriched compared to its host star. NGTS-30 b/TOI-4862 b is one of the youngest well-characterised long-period exoplanets found to date and will therefore be important in the quest to understanding the formation and evolution of exoplanets across the full range of orbital separations and ages.

Comments:18 pages, 14 figures, accepted for publication in A&ASubjects:Earth and Planetary Astrophysics (astro-ph.EP)Cite as:[arXiv:2404.02974](https://arxiv.org/abs/2404.02974) \[astro-ph.EP\](or [arXiv:2404.02974v1](https://arxiv.org/abs/2404.02974v1) \[astro-ph.EP\] for this version)
[https://doi.org/10.48550/arXiv.2404.02974](https://doi.org/10.48550/arXiv.2404.02974)

Focus to learn more

arXiv-issued DOI via DataCite

## Submission history

From: Matthew Battley \[ [view email](/show-email/c46e0dda/2404.02974)\]

**\[v1\]**
Wed, 3 Apr 2024 18:00:48 UTC (4,694 KB)

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