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We investigate an in-situ formation scenario for Earth-mass terrestrialplanets in short-period, potentially habitable orbits around low-mass stars(M_star < 0.3 M_sun). We then investigate the feasibility of detecting theseEarth-sized planets. Our simulations of terrestrial planet formation follow thegrowth of planetary embryos in an annular region around a fiducial M7 primary.Our simulations couple a semi-analytic model to a full N-body integration tofollow the growth from ~3x10^21 g to the final planetary system configurationsthat generally consist of 3-5 planets with masses of order 0.1 - 1.0 M_earth inor near the habitable zone of the star. To obtain a concrete estimate of thedetectability of the planets arising in our simulations, we present a detailedMonte-Carlo transit detection simulation. We find that detection of 1 R_earthplanets around the local M-dwarfs is challenging for a 1m class ground-basedphotometric search, but that detection of planets of larger radius is adistinct possibility. The detection of Earth-sized planets is straightforward,however, with an all-sky survey by a low-cost satellite mission. Given areduced correlated noise level of 0.45 mmag and an intermediate planetaryice-mass fraction of planets orbiting a target list drawn from the nearestlate-type M dwarfs, a ground-based photometric search could detect, on average,0.8 of these planets with an extended search. A space-based photometric search(similar to the TESS mission) should discover ~17 of these Earth-sized planetsduring it's two year survey, with an assumed occurrence fraction of 28%.

Formation and Detection of Earth Mass Planets around Low Mass Stars