Planets orbiting M-dwarf stars are prime targets in the search for rocky exoplanet atmospheres. The small size of M dwarfs renders their planets exceptional transmission spectroscopy, facilitating atmospheric characterization. However, it remains unknown whether host stars' highly variable extreme-UV radiation environments allow atmospheres to persist. With JWST, we have begun determine or not ...

We analyze the MOA-2020-BLG-208 gravitational microlensing event and present discovery characterization of a new planet, MOA-2020-BLG-208Lb, with an estimated sub-Saturn mass. With mass ratio $q = 3.17^{+0.28}_{-0.26} \times 10^{-4}$ separation $s 1.3807^{+0.0018}_{-0.0018}$, planet lies near peak mass-ratio function derived by MOA collaboration (Suzuki et al. 2016), edge expected sample sensit...

Terrestrial planets are easier to detect around M dwarfs than other types of stars, making them promising for next-generation atmospheric characterization studies. The $TESS$ mission has greatly increased the number known dwarf that we can use perform population studies, allowing us explore how rocky planet occurrence rate varies with host radius, following in footsteps past work $Kepler$ data....

The system of two transiting Neptune-sized planets around the bright, young M-dwarf AU Mic provides a unique opportunity to test models planet formation, early evolution, and star-planet interaction. However, intense magnetic activity host star makes measuring masses via radial velocity (RV) method very challenging. We report on 1-year, intensive monitoring campaign using 91 observations with H...

We report the light-curve analysis for event MOA-2020-BLG-135, which leads to discovery of a new Neptune-class planet, MOA-2020-BLG-135Lb. With derived mass ratio $q=1.52_{-0.31}^{+0.39} \times 10^{-4}$ and separation $s\approx1$, planet lies exactly at break likely peak exoplanet mass-ratio function by MOA collaboration (Suzuki et al. 2016). estimate properties lens system based on Galactic mo...

We present the discovery and characterisation of two transiting planets observed by \textit{TESS} in light curves young bright (V=9.67) star HD73583 (TOI-560). perform an intensive spectroscopic photometric space- ground-based follow-up order to confirm characterise system. found that is a ($\sim 500$~Myr) active with rotational period $12.08 \pm 0.11 $\,d, mass radius $ 0.73 0.02 M_\odot$ $0.6...

Consider the field F2n . Its elements are presented as polynomials from F2[x] modulo some irreducible polynomial of degree n. This polynomial can be found in time polynomial in n, as well as the matrix that related two representation corresponding to different irreducible polynomials [2]. Therefore, we do not need to specify a choice of the irreducible polynomial speaking about polynomial reduc...

In this article, we consider the equation

Since planet occurrence and primordial atmospheric retention probability increase with period, the occurrence-weighted median planets discovered by transit surveys may bear little resemblance to low-occurrence, short-period sculpted escape ordinarily used calibrate mass--radius relations formation models. An relation for low-mass so far orbiting solar-type stars requires both Earth-mass Neptune...

55 Cnc e is a transiting super-Earth (radius $1.88\rm\,R_\oplus$ and mass $8\rm\, M_\oplus$) orbiting G8V host star on 17-hour orbit. Spitzer observations of the planet's phase curve at 4.5 $\mu$m revealed time-varying occultation depth, MOST optical are consistent with amplitude offset maximum light. Both broadband high-resolution spectroscopic analyses either high mean molecular weight atmosp...