Exoplanet X-ray irradiation and evaporation rates with eROSITA

Foster, G.; Poppenhaeger, Katja; Ilic, N.; Schwope, A. D.

doi:10.1051/0004-6361/202141097

Cited by 20 publications

(12 citation statements)

References 80 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For computing F XUV and Ṁb , we used the procedures of Sanz-Forcada et al (2011). Although the mass loss rate during the first stages of evolution of the host star was necessarily greater (Ribas et al 2005;Kubyshkina et al 2018), the tabulated upper limit of present-day Ṁb translates into 0.07 M ⊕ Ga −1 , which is comparable or relatively low in comparison with many transiting exoplanets with atmospheres investigated to date (e.g., K2-100 b with more than 0.5 M ⊕ Ga −1 , Barragán et al 2019; TOI-849 b with 0.95 M ⊕ Ga −1 , Armstrong et al 2020; Gl 436 b with 0.019 M ⊕ Ga −1 , Sanz-Forcada et al 2011;Villarreal D'Angelo et al 2021;Foster et al 2022; see Fig. 11 of the latter authors for a population study).…”

Section: Prospects For Atmospheric Characterisationmentioning

confidence: 96%

A detailed analysis of the Gl 486 planetary system

Caballero

González-Álvarez

Brady

et al. 2022

A&A

View full text Add to dashboard Cite

Context. The Gl 486 system consists of a very nearby, relatively bright, weakly active M3.5 V star at just 8 pc with a warm transiting rocky planet of about 1.3 R ⊕ and 3.0 M ⊕ that is ideal for both transmission and emission spectroscopy and for testing interior models of telluric planets. Aims. To prepare for future studies, we thoroughly characterise the planetary system with new accurate and precise data collected with state-ofthe-art photometers from space and spectrometers and interferometers from the ground. Methods. We collected light curves of seven new transits observed with the CHEOPS space mission and new radial velocities obtained with MAROON-X at the 8.1 m Gemini North and CARMENES at the 3.5 m Calar Alto telescopes, together with previously published spectroscopic and photometric data from the two spectrographs and TESS. We also performed near-infrared interferometric observations with the CHARA Array and new photometric monitoring with a suite of smaller telescopes (AstroLAB, LCOGT, OSN, TJO). This extraordinary and rich data set was the input for our comprehensive analysis. Results. From interferometry, we measure a limb-darkened disc angular size of the star Gl 486 at θ LDD = 0.390 ± 0.018 mas. Together with a corrected Gaia EDR3 parallax, we obtain a stellar radius R = 0.339 ± 0.015 R . We also measure a stellar rotation period at P rot = 49.9 ± 5.5 d, an upper limit to its XUV (5-920 Å) flux with new Hubble/STIS data, and, for the first time, a variety of element abundances (Fe, Mg, Si, V, Sr, Zr, Rb) and C/O ratio. Besides, we impose restrictive constraints on the presence of additional components, either stellar or substellar, in the system. With the input stellar parameters and the radial-velocity and transit data, we determine the radius and mass of the planet Gl 486 b at R p = 1.343 +0.063 −0.062 R ⊕ and M p = 3.00 +0.13 −0.13 M ⊕ , with relative uncertainties in planet radius and mass of 4.7 % and 4.2 %, respectively. From the planet parameters and the stellar element abundances, we infer the most probable models of planet internal structure and composition, which are consistent with a relatively small metallic core with respect to the Earth, a deep silicate mantle, and a thin volatile upper layer. With all these ingredients, we outline prospects for Gl 486 b atmospheric studies, especially with forthcoming James Webb Space Telescope observations.

show abstract

Section: Prospects For Atmospheric Characterisationmentioning

confidence: 96%

A detailed analysis of the Gl 486 planetary system

Caballero

González-Álvarez

Brady

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…It is thus reasonable to assume that log L x ≈ 28.5−30.0. Together with the mass and radius obtained for the planet, this gives a mass-loss range from 10 11 to 10 12 g s −1 (using the same relation as in Foster et al 2022). We used several assumptions mentioned in Foster et al (2022) and discussed in Poppenhaeger et al (2021).…”

Section: Atmospheric Erosionmentioning

confidence: 99%

“…We used several assumptions mentioned in Foster et al (2022) and discussed in Poppenhaeger et al (2021). This mass loss is rather high (Foster et al 2022). At this mass-loss rate, the planet would lose about one per cent or less of its mass in 100 Myr.…”

Section: Atmospheric Erosionmentioning

confidence: 99%

“…Complete erosion of the atmospheres of these planets is possible because V1298 Tau is a young active star, and the planets are small. GJ 143 is a nearby K dwarf (Dragomir et al 2019) of age 3.8 ± 3.7 Gyr characterised by log L x = 27.2 (Foster et al 2022). The outer planet GJ 143 b has a period of 35.6 days, a mass of M p = 22.7 +2.2 −1.9 M ⊕ (Dragomir et al 2019), and receives F X,pl = 16 erg s −1 cm −2 .…”

Section: Atmospheric Erosionmentioning

confidence: 99%

“…The outer planet GJ 143 b has a period of 35.6 days, a mass of M p = 22.7 +2.2 −1.9 M ⊕ (Dragomir et al 2019), and receives F X,pl = 16 erg s −1 cm −2 . Its mass-loss rate is only 5 × 10 7 g s −1 (Foster et al 2022). The inner planet GJ 143 c has an orbital period of 7.8 days and its mass is below 3.7 M ⊕ and it receives F X,pl = 123 erg s −1 cm −2 .…”

Section: Atmospheric Erosionmentioning

confidence: 99%

See 2 more Smart Citations

TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Šubjak¹,

Endl²,

Chaturvedi³

et al. 2022

A&A

View full text Add to dashboard Cite

We report the discovery of TOI-1268b, a transiting Saturn-mass planet from the TESS space mission. With an age of less than 1 Gyr, derived from various age indicators, TOI-1268b is the youngest Saturn-mass planet known to date; it contributes to the small sample of well-characterised young planets. It has an orbital period of P = 8.1577080 ± 0.0000044 days, and transits an early K-dwarf star with a mass of M* = 0.96 ± 0.04 M⊙, a radius of R* = 0.92 ± 0.06 R⊙, an effective temperature of Teff = 5300 ± 100 K, and a metallicity of 0.36 ± 0.06 dex. By combining TESS photometry with high-resolution spectra acquired with the Tull spectrograph at the McDonald Observatory, and the high-resolution spectrographs at the Tautenburg and Ondřejov Observatories, we measured a planetary mass of Mp = 96.4 ± 8.3 M⊕ and a radius of Rp = 9.1 ± 0.6 R⊕. TOI-1268 is an ideal system for studying the role of star-planet tidal interactions for non-inflated Saturn-mass planets. We used system parameters derived in this paper to constrain the planet’s tidal quality factor to the range of 104.5–5.3. When compared with the sample of other non-inflated Saturn-mass planets, TOI-1268b is one of the best candidates for transmission spectroscopy studies.

show abstract

Extrasolar Planets and Star-Planet Interaction

Poppenhaeger

2022

Handbook of X-Ray and Gamma-Ray Astrophysics

View full text Add to dashboard Cite

Exoplanet X-ray irradiation and evaporation rates with eROSITA

Cited by 20 publications

References 80 publications

A detailed analysis of the Gl 486 planetary system

A detailed analysis of the Gl 486 planetary system

TOI-1268b: The youngest hot Saturn-mass transiting exoplanet

Extrasolar Planets and Star-Planet Interaction

Contact Info

Product

Resources

About