Zobrazeno 1 - 10
of 45
pro vyhledávání: '"Pedersen, May G"'
Autor:
Crawford, Courtney L., Nikultsev, Nikita, Clayton, Geoffrey C., Tisserand, Patrick, Soon, Jamie, Pedersen, May G.
Hydrogen-deficient Carbon (HdC) stars are rare, low-mass, chemically peculiar, supergiant variables believed to be formed by a double white dwarf (DWD) merger, specifically of a Carbon/Oxygen- (CO-) and a Helium-white dwarf (He-WD). They consist of t
Externí odkaz:
http://arxiv.org/abs/2408.09700
Autor:
Pedersen, May G., Bell, Keaton J.
Given its large plate scale of 21" / pixel, analyses of data from the TESS space telescope must be wary of source confusion from blended light curves, which creates the potential to attribute observed photometric variability to the wrong astrophysica
Externí odkaz:
http://arxiv.org/abs/2304.05706
Autor:
Anders, Evan H., Pedersen, May G.
Publikováno v:
Galaxies 2023, 11(2), 56
The convective envelopes of solar-type stars and the convective cores of intermediate- and high-mass stars share boundaries with stable radiative zones. Through a host of processes we collectively refer to as "convective boundary mixing" (CBM), conve
Externí odkaz:
http://arxiv.org/abs/2303.12099
Autor:
Pedersen, May G.
One of the largest uncertainties in stellar structure and evolution theory is the transport of angular momentum in the stellar interiors. Asteroseismology offers a powerful tool for measuring the internal rotation frequencies of pulsating stars, but
Externí odkaz:
http://arxiv.org/abs/2208.14497
Autor:
Cotton, Daniel V., Buzasi, Derek L., Aerts, Conny, Bailey, Jeremy, Burssens, Siemen, Pedersen, May G., Stello, Dennis, Kedziora-Chudczer, Lucyna, De Horta, Ain, De Cat, Peter, Lewis, Fiona, Malla, Sai Prathyusha, Wright, Duncan J., Bott, Kimberly
Publikováno v:
Nature Astronomy, Vol 6, pages 154-164 (2022)
Here we report the detection of polarization variations due to nonradial modes in the beta Cephei star beta Crucis. In so doing we confirm 40-year-old predictions of pulsation-induced polarization variability and its utility in asteroseismology for m
Externí odkaz:
http://arxiv.org/abs/2205.11679
Autor:
Pedersen, May G.
The chemical evolution of the Galaxy is largely guided by the yields from massive stars. Their evolution is heavily influenced by their internal mixing, allowing the stars to live longer and yield a more massive helium core at the end of their main-s
Externí odkaz:
http://arxiv.org/abs/2203.02046
Autor:
Van Beeck, Jordan, Bowman, Dominic M., Pedersen, May G., Van Reeth, Timothy, Van Hoolst, Tim, Aerts, Conny
Publikováno v:
A&A 655, A59 (2021)
Context. Slowly pulsating B (SPB) stars are main-sequence multi-periodic oscillators that display non-radial gravity modes. For a fraction of these pulsators, 4-year photometric light curves obtained with the Kepler space telescope reveal period spac
Externí odkaz:
http://arxiv.org/abs/2108.02907
Autor:
Pedersen, May G., Aerts, Conny, Pápics, Péter I., Michielsen, Mathias, Gebruers, Sarah, Rogers, Tamara M., Molenberghs, Geerts, Burssens, Siemen, Garcia, Stefano, Bowman, Dominic M.
During most of their life, stars fuse hydrogen into helium in their cores. The mixing of chemical elements in the radiative envelope of stars with a convective core is able to replenish the core with extra fuel. If effective, such deep mixing allows
Externí odkaz:
http://arxiv.org/abs/2105.04533
Autor:
Gebruers, Sarah, Straumit, Ilya, Tkachenko, Andrew, Mombarg, Joey S. G., Pedersen, May G., Van Reeth, Timothy, Li, Gang, Lampens, Patricia, Escorza, Ana, Bowman, Dominic M., De Cat, Peter, Vermeylen, Lore, Bodensteiner, Julia, Rix, Hans-Walter, Aerts, Conny
Publikováno v:
A&A 650, A151 (2021)
Asteroseismic modelling of the internal structure of main-sequence stars born with a convective core has so far been based on homogeneous analyses of space photometric Kepler light curves of 4 years duration, to which most often incomplete inhomogene
Externí odkaz:
http://arxiv.org/abs/2104.04521
Autor:
Serenelli, Aldo, Weiss, Achim, Aerts, Conny, Angelou, George C., Baroch, David, Bastian, Nate, Beck, Paul G., Bergemann, Maria, Bestenlehner, Joachim M., Czekala, Ian, Elias-Rosa, Nancy, Escorza, Ana, Van Eylen, Vincent, Feuillet, Diane K., Gandolfi, Davide, Gieles, Mark, Girardi, Leo, Lebreton, Yveline, Lodieu, Nicolas, Martig, Marie, Bertolami, Marcelo M. Miller, Mombarg, Joey S. G., Morales, Juan Carlos, Moya, Andres, Nsamba, Benard, Pavlovski, Kresimir, Pedersen, May G., Ribas, Ignasi, Schneider, Fabian R. N., Aguirre, Victor Silva, Stassun, Keivan G., Tolstoy, Eline, Tremblay, Pier-Emmanuel, Zwintz, Konstanze
The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exists a variety of methods in astronomy to
Externí odkaz:
http://arxiv.org/abs/2006.10868