Penev, Kaloyan
Permanent URI for this collectionhttps://hdl.handle.net/10735.1/6247
Kaloyan Penev joined the UTD faculty as an Assistant Professor of Physics in 2017. His research interests include:
- Extrasolar planet detection and orbital dynamics
- Searching for transiting extrasolar planets using small robotic telescopes
- High precision photometry from space and from the ground
- Orbital dynamics of extrasolar planetary systems
- Astrophysical probes of tidal dissipation in giant planets and low mass stars
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Browsing Penev, Kaloyan by Subject "Planetary systems"
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Item An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images(Institute of Physics Publishing, 2019-05) Rodriguez, J. E.; Quinn, S. N.; Huang, C. X.; Vanderburg, A.; Penev, Kaloyan; Brahm, R.; Jordán, A.; 0000-0003-4464-1371 (Penev, K); Penev, KaloyanWe report the discovery of TOI-172 b from the Transiting Exoplanet Survey Satellite (TESS) mission, a massive hot Jupiter transiting a slightly evolved G star with a 9.48-day orbital period. This is the first planet to be confirmed from analysis of only the TESS full frame images, because the host star was not chosen as a two-minute cadence target. From a global analysis of the TESS photometry and follow-up observations carried out by the TESS Follow-up Observing Program Working Group, TOI-172 (TIC 29857954) is a slightly evolved star with an effective temperature of T_{eff} = 5645 ± 50 K, a mass of M_{∗} = 1.128_{-0.061} ^{+0.065} M ⊙, radius of R_{∗} = 1.777_{-0.044} ^{+0.047} R ⊙, a surface gravity of log g_{∗} = 3.993 _{-0.028} ^{+0.027}, and an age of 7.4 _{-1.5} ^{+1.6}. Its planetary companion (TOI-172 b) has a radius of R _{P} = 0.965 _{-0.029} ^{+0.032} R_{J}, a mass of M _{P} = 5.42 _{-0.20} ^{+0.22} M _{J}, and is on an eccentric orbit (e = 0.3806 _{-0.0090} ^{+0.0093} ). TOI-172 b is one of the few known massive giant planets on a highly eccentric short-period orbit. Future study of the atmosphere of this planet and its system architecture offer opportunities to understand the formation and evolution of similar systems. © 2019. The American Astronomical Society. All rights reserved..Item HATS-39b, HATS-40b, HATS-41b, and HATS-42b: Three Inflated Hot Jupiters and a Super-Jupiter Transiting F Stars(Oxford Univ Press) Bento, J.; Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Penev, Kaloyan; Bayliss, D.; de Val-Borro, M.; Zhou, G.; Brahm, R.; Espinoza, N.; Rabus, M.; Jordan, A.; Suc, V.; Ciceri, S.; Sarkis, P.; Henning, T.; Mancini, L.; Tinney, C. G.; Wright, D. J.; Durkan, S.; Tan, T. G.; Lazar, J.; Papp, I.; Sari, P.; 0000-0003-4464-1371 (Penev, K); Penev, KaloyanWe report the discovery of four transiting hot Jupiters from the HATSouth survey: HATS39b, HATS-40b, HATS-41b, and HATS-42b. These discoveries add to the growing number of transiting planets orbiting moderately bright (12.5 ≲ V ≲ 13.7) F dwarf stars on short (2-5 d) periods. The planets have similar radii, ranging from 1.33{_{0.20}^{+0.29}} R_J for HATS-41b to 1.58{_{-0.12} ^{+0.16}} R_J for HATS-40b. Their masses and bulk densities, however, span more than an order of magnitude. HATS-39b has a mass of 0.63 ± 0.13M(J), and an inflated radius of 1.57 ± 0.12 R-J, making it a good target for future transmission spectroscopic studies. HATS41b is a very massive 9.7 ± 1.6M_J planet and one of only a few hot Jupiters found to date with a mass over 5 M_J. This planet orbits the highest metallicity star ([Fe/H] = 0.470 ± 0.010) known to host a transiting planet and is also likely on an eccentric orbit. The high mass, coupled with a relatively young age (1.34{_{-0.51} ^{+0.31}} Gyr) for the host star, is a factor that may explain why this planet's orbit has not yet circularized.