Here is a report on HZ exoplanets, numerous listed in Table 1 and stellar properties in Table 2.
A Catalog of Habitable Zone Exoplanets,
https://arxiv.org/abs/2210.02484
"The search for habitable planets has revealed many planets that can vary greatly from an Earth analog environment. These include highly eccentric orbits, giant planets, different bulk densities, relatively active stars, and evolved stars. This work catalogs all planets found to reside in the HZ and provides HZ boundaries, orbit characterization, and the potential for spectroscopic follow-up observations. Demographics of the HZ planets are compared with a full catalog of exoplanets. Extreme planets within the HZ are highlighted, and how their unique properties may affect their potential habitability. Kepler-296 f is the most eccentric <2 R⊕ planet that spends 100% of its orbit in the HZ. HD 106270 b and HD 38529 c are the most massive planets (<13 MJ) that orbit within the HZ, and are ideal targets for determining the properties of potential hosts of HZ exomoons. These planets, along with the others highlighted, will serve as special edge-cases to the Earth-based scenario and observations of these targets will help test the resilience of habitability outside the standard model. The most promising observational targets are HD 102365 b and 55 Cnc f, and the best candidates that are <2 R⊕ are GJ 667 C c, Wolf 1061 c, Teegarden's Star b, and Proxima Cen b."
ref paper, 33-pages,
https://arxiv.org/pdf/2210.02484.pdf, draft 07-Oct-2022.
From the PDF report, “1. INTRODUCTION Exoplanet discoveries over the past several decades have revealed a vast diversity of planetary architectures (Ford 2014; Winn & Fabrycky 2015), and shown that terrestrial planets are far more common than their giant planet counterparts (Borucki 2016). In these ongoing exoplanet searches, discovering those planets that may harbor life has been a primary objective for the astrobiology community (Fujii et al. 2018; Schwieterman et al. 2018; Glaser et al. 2020; Lisse et al. 2020). A potential pathway toward the identification of such worlds is to constrain the stellar and planetary parameter space that may allow for the presence of surface liquid water. Such is the premise of the habitable zone (HZ), defined as the region around a star where water can exist in a liquid state on the surface of a planet with sufficient atmospheric pressure (Kasting et al. 1993; Kopparapu et al. 2013, 2014; Kane et al. 2016). The HZ broadly consists of two main regions; the conservative habitable zone (CHZ) and the optimistic habitable zone (OHZ), shown in Figure 1 as the light green and dark green regions, respectively. The CHZ inner boundary is the runaway greenhouse limit, during which water loss can occur through photodissociation of water molecules in the upper atmosphere. The CHZ outer boundary is the maximum greenhouse, where the planetary temperature conditions allow condensation of substantial atmospheric CO2 on the surface (Kopparapu et al. 2013). The OHZ inner boundary, the Recent Venus limit, is based on the empirical observation that the surface of Venus has been dry for at least a billion years, but may have had conditions suitable for surface liquid water prior (Kane et al. 2014; Way et al. 2016). The outer edge of the OHZ, the Early Mars limit, is based on evidence that Mars appears to have harbored surface liquid water ~ 3.8 Gya (Kopparapu et al. 2013).”
My note. “Table 1. Habitable Zone Planet Properties.”, and “Table 2. Stellar Properties.”, lists many dozens in the tables.
"5. CONCLUSIONS In this paper, we present a complete catalog (at time of writing) of planets that orbit within or through the HZ, including the HZ boundaries and the percentage of the orbital period that each planet spends in their star's HZ. Observational metrics for each planet, such as TSM values and RV amplitude, are included to facilitate selection for future follow-up observations."
Some may be interested in reading this report.
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