arXiv subjects

Stefano Meschiari

Publications and source records attributed to Stefano Meschiari.

22 records · Page 2Linked to original sources

arXiv2009

A long-period planet orbiting a nearby Sun-like star

The Doppler wobble induced by the extra-solar planet HD 134987b was first detected by data from the Keck Telescope nearly a decade ago, and was subsequently confirmed by data from the Anglo-Australian Telescope. However, as more data have been acquired for this star over the years since, the quality of a single Keplerian fit to that data has been getting steadily worse. The best fit single Keplerian to the 138 Keck and AAT observations now in hand has an root-mean-square (RMS) scatter of 6.6 m/s. This is significantly in excess of both the instrumental precision achieved by both the Keck and Anglo-Australian Planet Searches for stars of this magnitude, and of the jitter expected for a star with the properties of HD134987. However, a double Keplerian (i.e. dual planet) fit delivers a significantly reduced RMS of 3.3 m/s. The best-fit double planet solution has minimum planet masses of 1.59 and 0.82Mjup, orbital periods of 258 and 5000d, and eccentricities of 0.23 and 0.12 respectively. We find evidence that activity-induced jitter is a significant factor in our fits and do not find evidence for asteroseismological p-modes. We also present seven years of photometry at a typical precision of 0.003mag with the T8 0.8m automatic photometric telescope at Fairborn observatory. These observations do not detect photometric variability and support the inference that the detected radial-velocity periods are due to planetary mass companions rather than due to photospheric spots and plages.

astro-ph.SR↗

arXiv2009

Systemic: A Testbed For Characterizing the Detection of Extrasolar Planets. I. The Systemic Console Package

We present the systemic Console, a new all-in-one, general-purpose software package for the analysis and combined multiparameter fitting of Doppler radial velocity (RV) and transit timing observations. We give an overview of the computational algorithms implemented in the Console, and describe the tools offered for streamlining the characterization of planetary systems. We illustrate the capabilities of the package by analyzing an updated radial velocity data set for the HD128311 planetary system. HD128311 harbors a pair of planets that appear to be participating in a 2:1 mean motion resonance. We show that the dynamical configuration cannot be fully determined from the current data. We find that if a planetary system like HD128311 is found to undergo transits, then self-consistent Newtonian fits to combined radial velocity data and a small number of timing measurements of transit midpoints can provide an immediate and vastly improved characterization of the planet's dynamical state.

astro-ph.EP↗

arXiv2009

A Quasi-Stationary Solution to Gliese 436b's Eccentricity

We investigate the possibility that the large orbital eccentricity of the transiting Neptune-mass planet Gliese 436b is maintained in the face of tidal dissipation by a second planet in the system. We find that the currently observed configuration can be understood if Gliese 436b and a putative companion have evolved to a quasi-stationary fixed point in which the planets' orbital apses are co-linear and in which secular variations in the orbital eccentricities of the two planets have been almost entirely damped out. We adopt an octopole-order secular theory based on a Legendre expansion in the semi-major axis ratio to delineate well-defined regions of (P_c, M_c, e_c) space that can be occupied by a perturbing companion. We incorporate the evolutionary effect of tidal dissipation into our secular model of the system, and solve the resulting initial value problems for a large sample of the allowed configurations. We then polish the stationary configurations derived from secular theory with full numerical integrations. We present our results in the form of candidate companion planets to Gliese 436b. For these candidates, radial velocity half-amplitudes, K_c, are of order 3 m/s, and the maximum amplitude of orbit-to-orbit transit timing variations are of order Delta t=1 s to Delta t=5s. For the particular example case of a perturber with orbital period, P_c=40 d, mass, M_c=8.5 M_Earth, and eccentricity, e_c=0.58, we confirm our semi-analytic calculations with a full numerical 3-body integration of the orbital decay that includes tidal damping and spin evolution. Additionally, we discuss the possibility of many-perturber stationary configurations, utilizing modified Laplace-Lagrange secular theory.

astro-ph.EP↗

arXiv2008

The potential impact of groove modes on Type II planetary migration

In this letter, we briefly describe the evolution of a variety of self-gravitating protoplanetary disk models that contain annular grooves (e.g. gaps) in their surface density. These grooves are inspired by the density gaps that are presumed to open in response to the formation of a giant planet. Our work provides an extension of the previously studied groove modes that are known in the context of stellar disks. The emergence of spiral gravitational instabilities (GI) is predicted via a generalized eigenvalue code that performs a linear analysis, and confirmed with hydrodynamical simulations. We find the presence of a groove drives a fast-growing two-armed mode in moderately massive disks, and extends the importance of self-gravitating instabilities down to lower disk masses than for which they would otherwise occur. We discuss the potential importance of this instability in the context of planet formation, e.g. the modification of the torques driving Type II migration.

astro-ph↗