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Your search keyword '"Seager, S [0000-0002-6892-6948]"' showing total 4 results
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4 results on '"Seager, S [0000-0002-6892-6948]"'

1. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author

Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, M [0000-0001-9269-8060], Vanderburg, A [0000-0001-7246-5438], Huang, CX [0000-0003-0918-7484], Davis, MR [0000-0002-7451-4704], Affer, L [0000-0001-5600-3778], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Damasso, M [0000-0001-9984-4278], Dumusque, X [0000-0002-9332-2011], Fiorenzano, AFM [0000-0002-4272-4272], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Lienhard, F [0000-0003-4047-0771], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Pepe, F [0000-0002-9815-773X], Pinamonti, M [0000-0002-4445-1845], Poretti, E [0000-0003-1200-0473], Maldonado, J [0000-0002-2218-5689], Rice, K [0000-0002-6379-9185], Sozzetti, A [0000-0002-7504-365X], Wilson, TG [0000-0001-8749-1962], Udry, S [0000-0001-7576-6236], Baptista, J [0000-0002-9306-1704], Barkaoui, K [0000-0003-1464-9276], Becker, J [0000-0002-7733-4522], Benni, P [0000-0001-6981-8722], Bieryla, A [0000-0001-6637-5401], Bosch-Cabot, P [0000-0002-1514-5558], Ciardi, DR [0000-0002-5741-3047], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Dupuy, TJ [0000-0001-9823-1445], Goliguzova, MV [0000-0003-2228-7914], Guerra, P [0000-0002-4308-2339], Kraus, A [0000-0001-9811-568X], Lissauer, JJ [0000-0001-6513-1659], Huber, D [0000-0001-8832-4488], Murgas, F [0000-0001-9087-1245], Palle, E [0000-0003-0987-1593], Quinn, SN [0000-0002-8964-8377], Safonov, BS [0000-0003-1713-3208], Schwarz, RP [0000-0001-8227-1020], Shporer, A [0000-0002-1836-3120], Stassun, KG [0000-0002-3481-9052], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Ricker, GR [0000-0003-2058-6662], Seager, S [0000-0002-6892-6948], Vanderspek, R [0000-0001-6763-6562], Winn, J [0000-0002-4265-047X], Essack, Z [0000-0002-2482-0180], Lewis, HM [0000-0002-7871-085X], Rose, ME [0000-0003-4724-745X], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Exoplanet dynamics, FOS: Physical sciences, DAS, 5109 Space Sciences, Hot Neptunes, QB Astronomy, Transit photometry, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation

Published
2023
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2. TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

Author

Hobson, MJ, Jordán, A, Bryant, EM, Brahm, R, Bayliss, D, Hartman, JD, Bakos, GI, Henning, T, Almenara, JM, Barkaoui, K, Benkhaldoun, Z, Bonfils, X, Bouchy, F, Charbonneau, D, Cointepas, M, Collins, KA, Eastman, JD, Ghachoui, M, Gillon, M, Goeke, RF, Horne, K, Irwin, JM, Jehin, E, Jenkins, JM, Latham, DW, Moldovan, D, Murgas, F, Pozuelos, FJ, Ricker, GR, Schwarz, RP, Seager, S, Srdoc, G, Striegel, S, Timmermans, M, Vanderburg, A, Vanderspek, R, Winn, JN, Hobson, MJ [0000-0002-5945-7975], Jordán, A [0000-0002-5389-3944], Bryant, EM [0000-0001-7904-4441], Brahm, R [0000-0002-9158-7315], Bayliss, D [0000-0001-6023-1335], Hartman, JD [0000-0001-8732-6166], Bakos, GI [0000-0001-7204-6727], Henning, T [0000-0002-1493-300X], Almenara, JM [0000-0003-3208-9815], Barkaoui, K [0000-0003-1464-9276], Benkhaldoun, Z [0000-0001-6285-9847], Bonfils, X [0000-0001-9003-8894], Bouchy, F [0000-0002-7613-393X], Charbonneau, D [0000-0002-9003-484X], Collins, KA [0000-0001-6588-9574], Eastman, JD [0000-0003-3773-5142], Ghachoui, M [0000-0003-3986-0297], Gillon, M [0000-0003-1462-7739], Horne, K [0000-0003-1728-0304], Jehin, E [0000-0001-8923-488X], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Murgas, F [0000-0001-9087-1245], Pozuelos, FJ [0000-0003-1572-7707], Ricker, GR [0000-0003-2058-6662], Schwarz, RP [0000-0001-8227-1020], Seager, S [0000-0002-6892-6948], Vanderburg, A [0000-0001-7246-5438], Vanderspek, R [0000-0001-6763-6562], Winn, JN [0000-0002-4265-047X], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Space and Planetary Science, 5101 Astronomical Sciences, MCP, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M-dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry, and confirmed with radial velocities from ESPRESSO, and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of $\mathrm{0.665\pm0.025\,M_J}$ and a radius of $\mathrm{1.017\pm0.044\,R_J}$. It orbits close to its host star, with an orbital period of $\mathrm{2.5926\,d}$, but has an equilibrium temperature of $\mathrm{\approx 604 \, K}$, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of $\mathrm{0.3939\pm0.0030\,M_\odot}$, a radius of $\mathrm{0.3697\pm0.0018\,R_\odot}$, an effective temperature of $\mathrm{3389 \, K}$, and a J-band magnitude of $\mathrm{11.706\pm0.025}$. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M-dwarfs for atmospheric characterization., 15 pages, 4 figures. Accepted for publication in APJL

Published
2023

3. Complex Modulation of Rapidly Rotating Young M Dwarfs:Adding Pieces to the Puzzle

Author

Günther, Maximilian N., Berardo, David A., Ducrot, Elsa, Murray, Catriona A., Stassun, Keivan G., Olah, Katalin, Bouma, L. G., Rappaport, Saul, Winn, Joshua N., Feinstein, Adina D., Matthews, Elisabeth C., Sebastian, Daniel, Rackham, Benjamin V., Seli, Bálint, J. Triaud, Amaury H. M., Gillen, Edward, Levine, Alan M., Demory, Brice-Olivier, Gillon, Michaël, Queloz, Didier, Ricker, George R., Vanderspek, Roland K., Seager, Sara, Latham, David W., Jenkins, Jon M., Brasseur, C. E., Colón, Knicole D., Daylan, Tansu, Delrez, Laetitia, Fausnaugh, Michael, Garcia, Lionel J., Jayaraman, Rahul, Jehin, Emmanuel, Kristiansen, Martti H., Kruijssen, J. M. Diederik, Pedersen, Peter Pihlmann, Pozuelos, Francisco J., Rodriguez, Joseph E., Wohler, Bill, Zhan, Zhuchang, Günther, MN [0000-0002-3164-9086], Berardo, DA [0000-0001-6298-412X], Ducrot, E [0000-0002-7008-6888], Murray, CA [0000-0001-8504-5862], Stassun, KG [0000-0002-3481-9052], Olah, K [0000-0003-3669-7201], Bouma, LG [0000-0002-0514-5538], Rappaport, S [0000-0003-3182-5569], Winn, JN [0000-0002-4265-047X], Feinstein, AD [0000-0002-9464-8101], Matthews, EC [0000-0003-0593-1560], Sebastian, D [0000-0002-2214-9258], Rackham, BV [0000-0002-3627-1676], Seli, B [0000-0002-3658-2175], Amaury, AHM [0000-0002-5510-8751], Gillen, E [0000-0003-2851-3070], Levine, AM [0000-0001-8172-0453], Demory, BO [0000-0002-9355-5165], Gillon, M [0000-0003-1462-7739], Queloz, D [0000-0002-3012-0316], Ricker, GR [0000-0003-2058-6662], Vanderspek, RK [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Latham, DW [0000-0001-9911-7388], Jenkins, JM [0000-0002-4715-9460], Brasseur, CE [0000-0002-9314-960X], Colón, KD [0000-0001-8020-7121], Daylan, T [0000-0002-6939-9211], Delrez, L [0000-0001-6108-4808], Fausnaugh, M [0000-0002-9113-7162], Garcia, LJ [0000-0002-4296-2246], Jayaraman, R [0000-0002-7778-3117], Jehin, E [0000-0001-8923-488X], Kristiansen, MH [0000-0002-2607-138X], Kruijssen, JMD [0000-0002-8804-0212], Pedersen, PP [0000-0002-5220-609X], Pozuelos, FJ [0000-0003-1572-7707], Rodriguez, JE [0000-0001-8812-0565], Wohler, B [0000-0002-5402-9613], Zhan, Z [0000-0002-4142-1800], and Apollo - University of Cambridge Repository

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, Variable stars, 520 Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Stellar flares, Astrophysics::Cosmology and Extragalactic Astrophysics, M dwarf stars, Starspots, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, astro-ph.EP, Periodic variable stars, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, T Tauri stars, Stellar rotation, Pre-main sequence stars, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Stellar activity
Abstract

New sets of young M dwarfs with complex, sharp-peaked, and strictly periodic photometric modulations have recently been discovered with Kepler/K2 (scallop shells) and TESS (complex rotators). All are part of star-forming associations, are distinct from other variable stars, and likely belong to a unified class. Suggested hypotheses include star spots, accreting dust disks, co-rotating clouds of material, magnetically constrained material, spots and misaligned disks, and pulsations. Here, we provide a comprehensive overview and add new observational constraints with TESS and SPECULOOS Southern Observatory (SSO) photometry. We scrutinize all hypotheses from three new angles: (1) we investigate each scenario's occurrence rates via young star catalogs; (2) we study the features' longevity using over one year of combined data; and (3) we probe the expected color dependency with multi-color photometry. In this process, we also revisit the stellar parameters accounting for activity effects, study stellar flares as activity indicators over year-long time scales, and develop toy models to simulate typical morphologies. We rule out most hypotheses, and only (i) co-rotating material clouds and (ii) spots and misaligned disks remain feasible - with caveats. For (i), co-rotating dust might not be stable enough, while co-rotating gas alone likely cannot cause percentage-scale features; and (ii) would require misaligned disks around most young M dwarfs. We thus suggest a unified hypothesis, a superposition of large-amplitude spot modulations and sharp transits of co-rotating gas clouds. While the complex rotators' mystery remains, these new observations add valuable pieces to the puzzle going forward., Comment: Accepted in The Astronomical Journal, 23 pages, 14 figures, 2 tables. This is the authors' version of the manuscript

Published
2022
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4. HD 56414 b: A Warm Neptune Transiting an A-type Star

Author

Giacalone, S, Dressing, CD, Muñoz, AG, Hooton, MJ, Stassun, KG, Quinn, SN, Zhou, G, Ziegler, C, Vanderspek, R, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Briceño, C, Huang, CX, Rodriguez, DR, Shporer, A, Mann, AW, Watanabe, D, Wohler, B, Giacalone, S [0000-0002-8965-3969], Dressing, CD [0000-0001-8189-0233], Muñoz, AG [0000-0003-1756-4825], Hooton, MJ [0000-0003-0030-332X], Stassun, KG [0000-0002-3481-9052], Quinn, SN [0000-0002-8964-8377], Zhou, G [0000-0002-4891-3517], Ziegler, C [0000-0002-0619-7639], Vanderspek, R [0000-0001-6763-6562], Latham, DW [0000-0001-9911-7388], Seager, S [0000-0002-6892-6948], Winn, JN [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Briceño, C [0000-0001-7124-4094], Huang, CX [0000-0003-0918-7484], Rodriguez, DR [0000-0003-1286-5231], Shporer, A [0000-0002-1836-3120], Mann, AW [0000-0003-3654-1602], Watanabe, D [0000-0002-3555-8464], Wohler, B [0000-0002-5402-9613], Apollo - University of Cambridge Repository, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanet astronomy, Exoplanet evolution, FOS: Physical sciences, Astronomy and Astrophysics, 5109 Space Sciences, Transits, [SDU]Sciences of the Universe [physics], 5101 Astronomical Sciences, Space and Planetary Science, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery in TESS data and validation of HD 56414 b (a.k.a. TOI-1228 b), a Neptune-size ($R_{\rm p} = 3.71 \pm 0.20\, R_\oplus$) planet with a 29-day orbital period transiting a young (Age = $420 \pm 140$ Myr) A-type star in the TESS southern continuous viewing zone. HD 56414 is one of the hottest stars ($T_{\rm eff} = 8500 \pm 150 \, {\rm K}$) to host a known sub-Jovian planet. HD 56414 b lies on the boundary of the hot Neptune desert in planet radius -- bolometric insolation flux space, suggesting that the planet may be experiencing mass loss. To explore this, we apply a photoevaporation model that incorporates the high near ultraviolet continuum emission of A-type stars. We find that the planet can retain most of its atmosphere over the typical 1-Gyr main sequence lifetime of an A-type star if its mass is $\ge 8 \, M_\oplus$. Our model also predicts that close-in Neptune-size planets with masses $< 14 \, M_\oplus$ are susceptible to total atmospheric stripping over 1 Gyr, hinting that the hot Neptune desert, which has been previously observed around FGKM-type stars, likely extends to A-type stars., 12 pages, 4 figures, 1 table

Published
2022
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