Results 21 to 30 of about 79,370 (261)

On the chromospheric activity of stars with planets [PDF]

, 2011
Context. Signatures of chromospheric activity enhancement have been found for a dozen stars, pointing to a possible star-planet interaction. Nevertheless in the coronal activity regime, there is no conclusive observational evidence for such an ...
Alves, B. L. Canto Martins, Butler, de Medeiros, Fares, Flower, I. C. Leão, J. R. de Medeiros, Jetsu, Kashyap, Konacki, Konacki, L. P. de Souza Neto, M. L. das Chagas, Marcy, Mayor, Noyes, Poppenhaeger, S. Alves, Schmitt, Shkolnik, Shkolnik, Wright   +22 more
core   +2 more sources

Energetics of star–planet magnetic interactions

Astronomy & Astrophysics
Context. Star–planet magnetic interactions (SPMIs) occurring in the sub-Alfvénic regime can, in principle, induce stellar chromospheric hotspots. These hotspots could serve as observational markers for inferring key planetary properties, especially the ...
Paul Arghyadeep, Strugarek Antoine
doaj   +1 more source

A coordinated optical and X-ray spectroscopic campaign on HD179949: searching for planet-induced chromospheric and coronal activity [PDF]

, 2013
HD179949 is an F8V star, orbited by a close-in giant planet with a period of ~3 days. Previous studies suggested that the planet enhances the magnetic activity of the parent star, producing a chromospheric hot spot which rotates in phase with the planet ...
Bohlender, D., Cameron, A. C., Dieters, S., Donati, J. -F., Fares, R., Fiorenzano, A. F. Martìnez, Jardine, M., Lanza, A. F., Maggio, A., Moutou, C., Pagano, I., Scandariato, G., Shkolnik, E. L.   +12 more
core   +4 more sources

Classification of magnetized star--planet interactions: bow shocks, tails, and inspiraling flows

, 2015
Close-in exoplanets interact with their host stars gravitationally as well as via their magnetized plasma outflows. The rich dynamics that arises may result in distinct observable features.
Königl, Arieh, Matsakos, Titos, Uribe, Ana   +2 more
core   +3 more sources

Planet-star interactions with precise transit timing

Astronomy & Astrophysics
Context. Giant exoplanets on 1-3 day orbits, known as ultra-hot Jupiters, induce detectable tides in their host stars. The energy of those tides dissipates at a rate related to the properties of the stellar interior. At the same time, a planet loses its orbital angular momentum and spirals into the host star.
G. Maciejewski, J. Golonka, M. Fernández, J. Ohlert, V. Casanova, D. Pérez Medialdea   +5 more
openaire   +2 more sources

Wide Binary Orbits Are Preferentially Aligned with the Orbits of Small Planets, but Probably Not Hot Jupiters

The Astronomical Journal
Studying the relative orientations of the orbits of exoplanets and wide-orbiting binary companions (semimajor axis greater than 100 au) can shed light on how planets form and evolve in binary systems. Previous observations by multiple groups discovered a
Sam Christian, Andrew Vanderburg, Juliette Becker, Adam L. Kraus, Logan Pearce, Karen A. Collins, Malena Rice, Eric L. N. Jensen, David Baker, Valerio Bozza, Paul Benni, Allyson Bieryla, Avraham Binnenfeld, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Phil Evans, Marshall C. Johnson, Eric Girardin, Joao Gregorio, Pablo Lewin, Tsevi Mazeh, Felipe Murgas, Aviad Panahi, Francisco J. Pozuelos, Don J. Radford, Howard M. Relles, Fabian Rodriguez Frustaglia, Richard P. Schwarz, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, William C. Waalkes, Gavin Wang, Justin Wittrock, Shay Zucker   +35 more
doaj   +1 more source

Star-planet interactions [PDF]

, 2014
Stars interact with their planets through gravitation, radiation, and magnetic fields. I shall focus on the interactions between late-type stars with an outer convection zone and close-in planets, i.e., with an orbital semimajor axis smaller than ...
Lanza, A. F.
core   +1 more source

Tidal evolution of close-in giant planets : Evidence of Type II migration?

, 2012
It is well accepted that 'hot Jupiters' did not form in situ, as the temperature in the protoplanetary disc at the radius at which they now orbit would have been too high for planet formation to have occurred. These planets, instead, form at larger radii
A. Collier Cameron, Alibert, Armitage, Armitage, Barnes, Bell, Benítez-LLamby, Bouvier, Brown, Chabrier, Collier Cameron, Collier Cameron, D'Angelo, Davis, Dobbs-Dixon, Eggleton, Faber, Fabrycky, Ford, Ford, Goldreich, Hansen, Herbst, Ida, J. Veljanoski, Jackson, Kozai, Kuchner, Königl, Lin, Lin, Marcy, Mardling, Marzari, Matsumura, Mayor, Mestel, Morton, Nagasawa, Pont, Queloz, Rasio, Rice, Triaud, Trilling, Udry, W. K. M. Rice, Ward, Winn, Winn, Wright, Wu   +51 more
core   +2 more sources

Overview of molecular signatures of senescence and associated resources: pros and cons

FEBS Open Bio, EarlyView.
Cells can enter a stress response state termed cellular senescence that is involved in various diseases and aging. Detecting these cells is challenging due to the lack of universal biomarkers. This review presents the current state of senescence identification, from biomarkers to molecular signatures, compares tools and approaches, and highlights ...
Orestis A. Ntintas, Sylvia Vagena, Pavlos Pantelis, Giorgos Theocharous, Russel Petty, Konstantinos Evangelou, Vassilis G. Gorgoulis   +6 more
wiley   +1 more source

Magnetic Effect on the Evolution of an Eccentric and Inclined Orbit

The Astrophysical Journal
We provide a method to calculate the evolution of an eccentric and inclined orbit under the magnetic effect. Taking the unipolar interaction as an example, we study both coplanar and inclined orbits. We calculate the Lorentz force and then the changes in
Xing Wei
doaj   +1 more source