Zobrazeno 1 - 10
of 122
pro vyhledávání: '"Lee, Eve J."'
Autor:
Boley, Kiersten M., Christiansen, Jessie L., Zink, Jon, Hardegree-Ullman, Kevin, Lee, Eve J., Hopkins, Philip F., Wang, Ji, Fernandes, Rachel B., Bergsten, Galen J., Bhure, Sakhee
Planet formation is expected to be severely limited in disks of low metallicity, owing to both the small solid mass reservoir and the low opacity accelerating the disk gas dissipation. While previous studies have found a weak correlation between the
Externí odkaz:
http://arxiv.org/abs/2407.13821
Autor:
Lee, Eve J.
How rapidly a planet grows in mass and how far they may park from the host star depend sensitively on two non-dimensional parameters: Stokes number St and turbulent $\alpha$. Yet, these parameters remain highly uncertain being difficult or impossible
Externí odkaz:
http://arxiv.org/abs/2407.02568
Autor:
Chachan, Yayaati, Dalba, Paul A., Thorngren, Daniel P., Kane, Stephen R., Lee, Eve J., Schwieterman, Edward W., Isaacson, Howard, Howard, Andrew W., Payne, Matthew J.
Systems hosting multiple giant planets are important laboratories for understanding planetary formation and migration processes. We present a nearly decade-long Doppler spectroscopy campaign from the Keck-I telescope to characterize the two transitin
Externí odkaz:
http://arxiv.org/abs/2405.11017
Autor:
Bryan, Marta L., Lee, Eve J.
The connection between outer gas giants and inner super-Earths reflects their formation and evolutionary histories. Past work exploring this link has suggested a tentative positive correlation between these two populations, but these studies have bee
Externí odkaz:
http://arxiv.org/abs/2403.08873
Autor:
Crotts, Katie A., Matthews, Brenda C., Duchêne, Gaspard, Esposito, Thomas M., Dong, Ruobing, Hom, Justin, Oppenheimer, Rebecca, Rice, Malena, Wolff, Schuyler G., Chen, Christine H., Ó, Clarissa R. Do, Kalas, Paul, Lewis, Briley L., Weinberger, Alycia J., Wilner, David J., Ammons, Mark, Arriaga, Pauline, De Rosa, Robert J., Debes, John H., Fitzgerald, Michael P., Gonzales, Eileen C., Hines, Dean C., Hinkley, Sasha, Hughes, A. Meredith, Kolokolova, Ludmilla, Lee, Eve J., López, Ronald A., Macintosh, Bruce, Mazoyer, Johan, Metchev, Stanimir, Millar-Blanchaer, Maxwell A., Nielsen, Eric L., Patience, Jenny, Perrin, Marshall D., Pueyo, Laurent, Rantakyrö, Fredrik T., Ren, Bin B., Schneider, Glenn, Soummer, Remi, Stark, Christopher C.
The Gemini Planet Imager (GPI) has excelled in imaging debris disks in the near-infrared. The GPI Exoplanet Survey (GPIES) imaged twenty-four debris disks in polarized $H$-band light, while other programs observed half of these disks in polarized $J$
Externí odkaz:
http://arxiv.org/abs/2311.14599
Autor:
Savignac, Vincent, Lee, Eve J.
Super-Earths and mini-Neptunes are the most common types of exoplanets discovered, yet the physics of their formation are still debated. Standard core accretion models in gas-rich environment find that typical mini-Neptune mass planets would blow up
Externí odkaz:
http://arxiv.org/abs/2310.06013
Autor:
Chachan, Yayaati, Lee, Eve J.
Current measurements of planet population as a function of stellar mass show three seemingly contradictory signatures: close-in super-Earths are more prevalent around M dwarfs than FGK dwarfs; inner super-Earths are correlated with outer giants; and
Externí odkaz:
http://arxiv.org/abs/2305.00803
The hot Saturn population exhibits a boundary in mass-radius space, such that no planets are observed at a density less than $\sim$0.1 g cm$^{-3}$. Yet, planet interior structure models can readily construct such objects as the natural result of radi
Externí odkaz:
http://arxiv.org/abs/2211.11770
Radio images of protoplanetary disks demonstrate that dust grains tend to organize themselves into rings. These rings may be a consequence of dust trapping within gas pressure maxima wherein the local high dust-to-gas ratio is expected to trigger the
Externí odkaz:
http://arxiv.org/abs/2206.01219
The observed exoplanet population features a gap in the radius distribution that separates the smaller super-Earths ($\lesssim$1.7 Earth radii) from the larger sub-Neptunes ($\sim$1.7--4 Earth radii). While mass loss theories can explain many of the
Externí odkaz:
http://arxiv.org/abs/2201.09898