CHEOPS and TESS view of the ultra-short-period super-Earth TOI-561 b
Artikel i vetenskaplig tidskrift, 2023

Context. Ultra-short-period planets (USPs) are a unique class of super-Earths with an orbital period of less than a day, and hence they are subject to intense radiation from their host star. These planets cannot retain a primordial H/He atmosphere, and most of them are indeed consistent with being bare rocky cores. A few USPs, however, show evidence for a heavyweight envelope, which could be a water layer resilient to evaporation or a secondary metal-rich atmosphere sustained by outgassing of the molten volcanic surface. Much thus remains to be learned about the nature and formation of USPs. Aims. The prime goal of the present work is to refine the bulk planetary properties of the recently discovered TOI-561 b through the study of its transits and occultations. This is crucial in order to understand the internal structure of this USP and to assess the presence of an atmosphere. Methods. We obtained ultra-precise transit photometry of TOI-561 b with CHEOPS, and performed a joint analysis of these data along with three archival visits from CHEOPS and four TESS sectors. Results. Our analysis of TOI-561 b transit photometry put strong constraints on its properties. In particular, we restrict the uncertainties on the planetary radius at similar to 2% retrieving R-p = 1.42 +/- 0.02 R-circle plus. This result informs our internal structure modelling of the planet, which shows that the observations are consistent with a negligible H/He atmosphere; however, other lighter materials are required, in addition to a pure iron core and a silicate mantle, to explain the observed density. We find that this can be explained by the inclusion of a water layer in our model. Additionally, we ran a grid of forward models with a water-enriched atmosphere to explain the transit radius. We searched for variability in the measured R-p/R-star over time, which could trace changes in the structure of the planetary envelope. However, no temporal variations are recovered within the present data precision. In addition to the transit event, we tentatively detect an occultation signal in the TESS data with an eclipse depth L = 27.40(-11.35)(+10.87) ppm. We use models of outgassed atmospheres from the literature to explain this eclipse signal. We find that the thermal emission from the planet can mostly explain the observation. Based on this, we predict that near- to mid-infrared observations with the James Webb Space Telescope should be able to detect silicate species in the atmosphere of the planet. This could also reveal important clues about the planetary interior and help disentangle planet formation and evolution models.

planets and satellites: atmospheres

planets and satellites: composition

planets and satellites: individual: TOI-561 b

techniques: photometric

planets and satellites: terrestrial planets

Författare

J. A. Patel

Stockholms universitet

J. A. Egger

Universität Bern

T. G. Wilson

University of St Andrews

The University of Warwick

V. Bourrier

Université de Genève

L. Carone

Österreichische Akademie der Wissenschaften

M. Beck

Université de Genève

D. Ehrenreich

Université de Genève

S. G. Sousa

Universidade do Porto

W. Benz

Universität Bern

A. Brandeker

Stockholms universitet

A. Deline

Université de Genève

Y. Alibert

Universität Bern

K. W. F. Lam

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

M. Lendl

Université de Genève

R. Alonso

Universidad de la Laguna

Instituto de Astrofísica de Canarias

G. Anglada

Institut d'Estudis Espacials de Catalunya (IEEC)

Consejo Superior de Investigaciones Científicas (CSIC)

T. Barczy

Admatis

D. Barrado

Consejo Superior de Investigaciones Científicas (CSIC)

S. C. C. Barros

Universidade do Porto

W. Baumjohann

Österreichische Akademie der Wissenschaften

T. Beck

Universität Bern

N. Billot

Université de Genève

X. Bonfils

Université Grenoble Alpes

C. Broeg

Universität Bern

M. -d. Busch

Universität Bern

J. Cabrera

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

S. Charnoz

Université Paris Descartes

A. Collier Cameron

University of St Andrews

Sz. Csizmadia

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

M. B. Davies

Lunds universitet

M. Deleuil

Aix-Marseille Université

L. Delrez

Universite de Liège

O. D. S. Demangeon

Universidade do Porto

B. -o. Demory

Universität Bern

A. Erikson

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

A. Fortier

Universität Bern

L. Fossati

Österreichische Akademie der Wissenschaften

Malcolm Fridlund

Universiteit Leiden

Chalmers, Rymd-, geo- och miljövetenskap, Onsala rymdobservatorium

D. Gandolfi

Universita degli Studi di Torino

M. Gillon

Universite de Liège

M. Guedel

Universität Wien

K. Heng

The University of Warwick

Universität Bern

S. Hoyer

Aix-Marseille Université

K. G. Isaak

Europeiska rymdorganisationen (ESA)

L. L. Kiss

Magyar Tudomanyos Akademia

Eötvös Loránd University (ELTE)

E. Kopp

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

J. Laskar

Sorbonne Université

A. Lecavelier des Etangs

Université Pierre et Marie Curie (UPMC)

C. Lovis

Université de Genève

D. Magrin

Istituto nazionale di astrofisica (INAF)

P. F. L. Maxted

Keele University

V. Nascimbeni

Istituto nazionale di astrofisica (INAF)

G. Olofsson

Stockholms universitet

R. Ottensamer

Universität Wien

I. Pagano

Istituto nazionale di astrofisica (INAF)

E. Palle

Instituto de Astrofísica de Canarias

G. Peter

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

G. Piotto

Università di Padova

Istituto nazionale di astrofisica (INAF)

D. Pollacco

The University of Warwick

D. Queloz

University of Cambridge

Eidgenössische Technische Hochschule Zürich (ETH)

R. Ragazzoni

Università di Padova

Istituto nazionale di astrofisica (INAF)

N. Rando

Europeiska rymdorganisationen (ESA)

F. Ratti

Europeiska rymdorganisationen (ESA)

H. Rauer

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

Freie Universität Berlin

Technische Universität Berlin

I. Ribas

Institut d'Estudis Espacials de Catalunya (IEEC)

Consejo Superior de Investigaciones Científicas (CSIC)

N. C. Santos

Universidade do Porto

G. Scandariato

Istituto nazionale di astrofisica (INAF)

D. Segransan

Université de Genève

A. E. Simon

Universität Bern

A. M. S. Smith

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

M. Steller

Österreichische Akademie der Wissenschaften

Gy. M. Szabo

Eötvös Loránd University (ELTE)

N. Thomas

Universität Bern

S. Udry

Université de Genève

B. Ulmer

Deutsches Zentrums für Luft- und Raumfahrt (DLR)

V. Van Grootel

Universite de Liège

V. Viotto

Istituto nazionale di astrofisica (INAF)

N. A. Walton

University of Cambridge

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 679 A92

Satellitstudier av exoplaneters mångfald

Rymdstyrelsen (174/18), 2019-02-04 -- 2023-08-01.

Exoplaneter från rymden - CHEOPS och PLATO, ESA's nästa två rymdteleskop (fas 2)

Rymdstyrelsen (65/19), 2020-01-01 -- 2022-12-31.

Rymdstyrelsen (177/19), 2020-01-01 -- 2022-12-31.

Ämneskategorier

Astronomi, astrofysik och kosmologi

Annan fysik

DOI

10.1051/0004-6361/202244946

Mer information

Senast uppdaterat

2024-01-09