2021
DOI: 10.3847/1538-3881/ac02bd
|View full text |Cite
|
Sign up to set email alerts
|

TKS X: Confirmation of TOI-1444b and a Comparative Analysis of the Ultra-short-period Planets with Hot Neptunes

Abstract: We report the discovery of TOI-1444b, a 1.4 R ⊕ super-Earth on a 0.47 day orbit around a Sun-like star discovered by TESS. Precise radial velocities from Keck/HIRES confirmed the planet and constrained the mass to be 3.87 ± 0.71M ⊕. The RV data set also indicates a possible nontransiting, 16 day planet (11.8 ± 2.9M ⊕). We report a tentative detection of phase-curve variation and a secondary eclipse of TOI-1444b in the TESS bandpass. TOI-1444b joins the grow… Show more

Help me understand this report

Search citation statements

Order By: Relevance

Paper Sections

Select...
3
2

Citation Types

5
23
0

Year Published

2021
2021
2024
2024

Publication Types

Select...
5
2

Relationship

0
7

Authors

Journals

citations
Cited by 22 publications
(31 citation statements)
references
References 114 publications
5
23
0
Order By: Relevance
“…Adibekyan et al (2012a) showed an over-abundance of magnesium for Neptune and super-Earth hosting stars, but these two populations were entangled within the same distribution for their comparison between hot-Jupiters, thus it is difficult to compare our results with theirs in this particular case. As with Dai et al (2021), we do see UHNs around stars enriched in iron compared to UHRs, with the one exception being the UHR exoplanet WASP-47 e, orbiting around an extremely iron-rich host ([Fe/H] = 0.45 ± 0.09). There does also seem to be a trend in UHNs being preferentially found around higher [Mg/Fe] stars compared to UHRs, but this trend for ultra-short exoplanets severely weakens out for the 𝛼-abundance (which is a combination of Ca, Mg, Ti and Al).…”
Section: Chemical Abundance Relationships Between Short Period and Ul...supporting
confidence: 70%
See 2 more Smart Citations
“…Adibekyan et al (2012a) showed an over-abundance of magnesium for Neptune and super-Earth hosting stars, but these two populations were entangled within the same distribution for their comparison between hot-Jupiters, thus it is difficult to compare our results with theirs in this particular case. As with Dai et al (2021), we do see UHNs around stars enriched in iron compared to UHRs, with the one exception being the UHR exoplanet WASP-47 e, orbiting around an extremely iron-rich host ([Fe/H] = 0.45 ± 0.09). There does also seem to be a trend in UHNs being preferentially found around higher [Mg/Fe] stars compared to UHRs, but this trend for ultra-short exoplanets severely weakens out for the 𝛼-abundance (which is a combination of Ca, Mg, Ti and Al).…”
Section: Chemical Abundance Relationships Between Short Period and Ul...supporting
confidence: 70%
“…Overall, there does not seem to be a statistical difference between the chemical properties of stars that host HNs and those that host HRs. Thus, following the conclusions of Dai et al (2021) and Winn et al (2017), our more robust chemical abundance results show that there is a possibility that short-period rocky worlds might be the remnant cores of hotter-gaseous Neptune worlds. The reason being is that there are only three of the 29 elemental abundances that had KS statistics significant enough to show that HRs and HNs come from different populations.…”
Section: Chemical Abundance Relationships Between Short Period and Ul...supporting
confidence: 70%
See 1 more Smart Citation
“…An additional discrepancy between the two studies is the mass of the USP planet, differing by almost a factor two. According to the W21 analysis, TOI-561 b has a mass of 3.2 ± 0.8 M ⊕ , making it consistent with a rocky composition and placing it among the population of typical small (< 2 R ⊕ ), extremely irradiated USP planets (Sanchis-Ojeda et al 2015;Dai et al 2021). Instead, assuming the low mass ( b = 1.59 ± 0.36 M ⊕ ) inferred from L21 analysis, TOI-561 b is not consistent with a pure rocky composition, and it is the lowest density USP super-Earth known to date, calling for a more complex interpretation (e.g.…”
Section: The Planetary Systemmentioning
confidence: 99%
“…An additional discrepancy between the two studies is the mass of the USP planet, differing by almost a factor two. According to the W21 analysis, TOI-561 b has a mass of 3.2 ± 0.8 M ⊕ , making it consistent with a rocky composition and placing it among the population of typical small (< 2 R ⊕ ), extremely irradiated USP planets (Sanchis-Ojeda et al 2015;Dai et al 2021). Instead, assuming the low mass (𝑀 b = 1.59 ± 0.36 M ⊕ ) inferred from L21 analysis, TOI-561 b is not consistent with a pure rocky composition, and it is the lowest density USP super-Earth known to date, calling for a more complex interpretation (e.g.…”
Section: The Planetary Systemmentioning
confidence: 99%