Potential climate and habitability of Gl 514 b
Authors: Biasiotti Lorenzo , Simonetti Paolo , Vladilo Giovanni , Ivanovski Stavro , Damasso Mario , Sozzetti Alessandro , Monai Sergio 
Published: July 2024

Introduction:&#160;&#160;The recently discovered super-Earth planet Gl 514 b, orbiting the nearby (7.6 pc, [1]) M-dwarf,&#160;is an interesting case to explore the habitability of planets that radically differ from the Earth. Habitability studies often rely on the classic definition of the Habitable Zone (HZ), and in particular on the so-called Conservative Habitable Zone (CHZ, [2]). Due to the combination of its relatively large semi-major axis (a=0.42 AU) and eccentricity (e=0.45), Gl 514b lies part of the time inside the CHZ (about 34% of the orbital period) and the rest of the time beyond the outer edge of the CHZ. This suggests the presence of strong seasonal variations that impact the actual habitability of the planet. Tracking the seasonal evolution of habitability is not possible using the HZ approach and requires the application of seasonal climate models tailored for specific stellar, orbital and planetary parameters.&#160;Investigating the potential climates of planets that exhibit seasonal episodes of habitability is intriguing because it could provide insights into the dynamic nature of planetary systems and the potential for the support of life in exotic&#160;scenarios. In this sense, the study of the habitability of Gl 514 b can be generalized to all that cases in which there are strong instellation variations, thus helping to define a &#8220;Seasonal Habitable Zone&#8221;.&#160;The Model:&#160;In our study we use the climate model, EOS-ESTM [3,4] for exploring the habitability of Gl 514 b by calculating an index of surface habitability based on the surface temperature distribution. In practice, we explore the habitability as a function of climate factors currently unconstrained by the observations (e.g., Fig 1), such as the ocean cover fraction, the obliquity, and the atmospheric composition. We consider three different types of atmospheres: (i) CO2-dominated, (ii) CO2&#160;+ 0.1% CH4&#160;and (iii) CO2&#160;+ 1.0% CH4.Since transits of Gl 514 b have not been detected so far, we estimate the radius and the surface gravity from interior structure models (e.g. [5]) and from the measurements of the minimum mass (5.2 M&#8853;). The high eccentricity of Gl 514 b suggests that the system is dynamically young and that spin-orbit tidal synchronization may not have yet occurred (e.g. [6]). Assuming that the planet is not tidally locked, in this contribution we present results obtained for a rotation of 1 day (see full paper for complete set of tests).&#160;Results:&#160;In the present work, we show&#160;how the habitability of Gl 514b is impacted by different combinations of&#160;planetary, orbital and atmospheric parameters. The impact of the ocean cover fraction is significant due to the orbit of Gl 514 b (see Figure 1).&#160;In fact, the large thermal capacity of even a 25-m shallow ocean provides sufficient thermal inertia to avoid freezing conditions near apoastron.&#160;Similarly, the obliquity plays a fundamental role in seasonal habitable events. The higher the obliquity of the planet, the greater the thermal excursion to the poles is (see Figure 2). Nonetheless, we show that these effects are regulated by the&#160;total surface pressure and the content of methane&#160;in the atmosphere. We present results of the parameter space that allows conditions of continuous and transient habitability.&#160;&#160;Figure 1. Predicted values of the habitability index, &#8462;, as a function of the ocean cover fraction and total surface pressure for three different atmosphericcompositions. Left panel: CO2-dominated; middle panel: CO2+ 0.1% CH4; right panel: CO2+ 1% CH4. For the remaining parameters we adopt &#120598; =23.44&#9702;,&#119875;&#119903;&#119900;&#119905;&#160;=1 day and &#120596;&#119901;&#119890;&#119903;&#119894;&#160;=0&#9702;. The dashed areas indicate the parameter space in which atmospheric CO2&#160;condensates.&#160;&#160;Figure 2. Seasonal and latitudinal maps of surface temperature obtained by extracting the results of Fig. 9c (case with 1% CH4) at constant values of axis obliquity (from left to right: &#120598; = 20&#9702;&#160;, 30&#9702;&#160;, 40&#9702;&#160;, 50&#9702;, and 60&#9702;) and total pressure (from top to bottom: &#119901;&#119905;&#119900;&#119905;&#160;=5 464, 3 593, 2 782, 2 154, and 1 668 mbar). The solid line indicate the limit within which water can be maintained in liquid form.&#160;Further investigations will include the impact of the host star on the exoplanet environment,&#160;especially concerning the photochemical reactions in the atmosphere driven by the large UV flux of the parent star. Apart from the direct impact on habitability due to its ionizing effects, the radiation environment of Gl 514 b may be conductive to the presence of high-altitude organic hazes that directly affect the climate state of the planet.&#160;Due to the proximity to Earth and the spectral class of the parent star, future observations of the emission and reflection spectra of Gl 514 b are expected to be possible with the E-ELT. In addition,&#160;asteroseismology obtained by extensive monitoring of nearby bright stars with PLATO&#160;may help to measure the age of Gl 514 and cast light on the evolutionary status of Gl 514 b. So far, we cannot completely exclude that the planet is transiting [7], in which case we would be able to constrain radius, mass and internal structure. Searches for transits might be performed with PLATO, during the &#8220;Step and stare&#8221; Observation Phase.These observations will allow us to test and constrain the models of planetary climate and habitability developed in our investigation.&#160;&#160;References:[1]&#160;Damasso M., et al., 2022, A&amp;A, 666, A187.[2]&#160;Kopparapu R. K., et al., 2013, ApJ, 765, 131.[3]&#160;Simonetti P., et al., 2022, ApJ, 925, 105.[4] Biasiotti L., et al., 2022, MNRAS, 514, 5105.[5] Fortney J. J., Marley M. S., Barnes J. W., 2007, ApJ, 659, 1661.[6]&#160;Barnes R., 2017, Celestial Mechanics and Dynamical Astronomy, 129, 509.[7]&#160;Damasso&#160;M., Nardiello D., 2022, Research Notes of the American Astronomical Society, 6, 184