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9 results for “Super Earth”
Most Super-Earths Have Less Than 3% Water: Mass-Radius Relations
<p>Mass-radius relations for rocky super-Earths, related to the models constructed in "Most Super-Earths Have Less Than 3% Water" by James G. Rogers, Caroline Dorn, Vivasvaan Aditya Raj, Hilke E. Schlichting, and Edward D. Young.</p> <p>We provide two .csv files for the scenarios of super-Earths with and without outgassed mantles, respectively. Each file contains planet masses and radii (measured in Earth units) under the scenario of stripped and retained steam atmospheres. These are provided for a range in total water mass fractions (X_H2O) and equilibrium temperature (Teq). Note that all models have an Earth-like 32.5 % iron-core mass fraction. The water mass fractions of stripped models are less than that of retained atmospheres.</p> <p>To extract a single mass-radius relation for a desired scenario, filter a file for planets of a given (retained) water mass fraction and equilibrium temperature. </p>
Data for: TOI-1685 b is a Hot Rocky Super-Earth (Burt et al. 2024)
<p>Machine Readable Tables containing the time series photometry and radial velocity data used in Burt et al. 2024 paper 'TOI-1685 b is a Hot Rocky Super-Earth: Updates to the Stellar and Planet Parameters of a Popular JWST Cycle 2 Target'</p> <p>Notes (also in ReadMe Document) </p> <p>TOI1685_Full_TimeSeries_Photometry_DataSet.dat : the juliet light curve input file for the transit fit presented in the paper.</p> <p>The nine columns in the file correspond to, Time (BJD_TDB), Normalized flux, Normalized flux error, Dataset label, Airmass, Centroid X offset, Centroid Y offset, PSF full-width half-maximum (FWHM) and PSF peak brightness. As these are not used to model the TESS light curves, these values are blank for the TESS data. For the MuSCAT2 data, entropy (a proxy for the PSF FWHM) is used in place of PSF FWHM, and PSF peak brightness is not used at set to 0. For the OMM data, total background across the target and comparison stars is used in place of PSF peak brightness. All values in the final five columns are normalized between -1 and 1 for any given dataset. </p> <p>~~~~~~~~~~~~~</p> <p>TOI1685_Full_RV_DataSet.csv : The full data sets from the MAROON-X data presented in this paper, as well as the CARMENES data from Bluhm et al. 2021 and the IRD data from Hirano et al. 2021. </p> <p>The fit presented in the paper only makes use of the RV time series from each instrument, but the SERVAL results for MAROON-X and CARMENES also provide a variety of activity indicators which we include as additional columns here for completeness.</p>
Formation of super-Earths in a protoplanetary disk
<p>This is a simulation of the process of formation for a planetary system with close-in super-Earths.</p> <p>The simulation begins with 125 planetary embryos, each with 0.4 times the mass of the Earth. The gray region shows the height of the protoplanetary disk. At the beginning of the simulation the embryos have strong gravitational encounters that increase their orbital inclinations (y-axis) and leads to collisions. After the embryos merge into larger bodies, interactions with the disk cause the eccentricities and inclinations to drop and the planets form a chain of mean motion resonances. Planets also experience torques from the disk that remove orbital angular momentum which causes the planets to drop to lower orbits. While the planets migrate through the disk, they accrete gas from the disk. The color of each body shows the fraction of their mass that is in the gaseous envelope.</p> <p>The disk dissipates after 5 Myr. With the disk gone, the planetary system becomes dynamically unstable and two new waves of giant impacts occur. This leaves behind a planetary system with larger planet masses, smaller gas envelopes, and higher mutual inclinations.</p>
Microlensing events indicate that super-Earth exoplanets are common in Jupiter-like orbits
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Data for: JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b
<p>Data and models accompanying the publication "JWST COMPASS: NIRSpec/G395H Transmission Observations of the Super-Earth TOI-836b". Here we include:</p> <ul> <li>Data, ExoTiC-JEDI light curves and transmission spectrum of JWST NIRSpec/G395H transit observations</li> <li>Data, Eureka! light curves and transmission spectrum of JWST NIRSpec/G395H transit observations</li> <li>Models, PICASO models and data shown in Figure 5</li> </ul> <p>Manuscript DOI: [] and [paper link]</p>
Data Products and Reduction Files For: JWST COMPASS: The 3-5 Micron Transmission Spectrum of the Super-Earth L 98-59 c
<p>Supplementary material for JWST COMPASS: The 3-5 Micron Transmission Spectrum of the Super-Earth L 98-59 c, Scarsdale et. al. 2024 (accepted). Included are:</p> <ol> <li>Control files necessary to reproduce the Eureka! reduction described in the paper</li> <li>Stage 4 (light curves) data products from Eureka!</li> <li>Final transmission spectra for the Eureka! and ExoTIC-JEDI reductions </li> </ol> <p>Please contact Nicholas Scarsdale (nscarsda at ucsc.edu) with any questions. </p>
Discovery of a Cold Giant Planet and Mass Measurement of a Hot Super-Earth in the Multi-Planetary System WASP-132 Supplementary Material
<p>Supplementary Material for the publication in Astronomy & Astrohpysics: Discovery of a Cold Giant Planet and Mass Measurement of a Hot Super-Earth in the Multi-Planetary System WASP-132.</p>
Birth cluster simulations of planetary systems with multiple super-Earths: initial conditions for white dwarf pollution drivers
<p>We provide the output parameters from our planetary system simulations around white dwarf main-sequence progenitors (1.5, 2.0 and 2.5 solar mass stars) embedded in a birth star cluster containing 8,000 stars. The data can serve the community as initial conditions for subsequent evolution simulations, e.g. to further investigate the role of eccentric planets in the pollution of white dwarfs. The planetary systems, consisting solely of super-Earths with 0.01 Jovian masses, were started in three different orbital configurations. The 3P model contains 3 planets with initial semimajor axes between 2.00 and 18.63 AU. We also simulated two 7-planet system models with different orbital spacing. The 7PC model represents a compact planetary system with 7 planets between 2.00 and 18.63 AU. The 7PW model represents a wide planetary system with 7 planets between 2.00 and 56.87 AU. The three planetary system models were distributed around 193 stars with 1.5 solar masses, around 114 stars with 2.0 solar masses and around 101 stars with 2.5 solar masses, and numerically integrated for 100 Myr considering the gravitational forces from the neighbouring stars in the star cluster.</p> <p>See the publication Stock et al. (2022) for further information.</p>
Arid or Cloudy: Characterizing the Atmosphere of the super-Earth 55 Cancri e using High-Resolution Spectroscopy
<p>These raw data and models are supplementary to the submission of the manuscript.</p>
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