Results 81 to 90 of about 1,140,165 (333)
The Missing Magnetic Morphology Term in Stellar Rotation Evolution [PDF]
, 2016 This study examines the relationship between magnetic field complexity and mass and angular momentum losses. Observations of open clusters have revealed a bimodal distribution of the rotation periods of solar-like stars that has proven difficult to ...
C. Garraffo, J. Drake, O. Cohen
semanticscholar +1 more source
First grids of low-mass stellar models and isochrones with self-consistent treatment of rotation [PDF]
Astronomy & Astrophysics, 2019 Aims.We present an extended grid of state-of-the art stellar models for low-mass stars including updated physics (nuclear reaction rates, surface boundary condition, mass-loss rate, angular momentum transport, rotation-induced mixing, and torque ...
L. Amard +6 more
semanticscholar +1 more source
Stellar ages and stellar rotation
, 2016 Stellar ages will play a big role in the next generation of astronomy. Useful to exoplaneteers and galactic archaeologists alike, this relatively under-exploited stellar property is currently limited by the precision of dating techniques. The work presented in this thesis contributes incrementally to a greater understanding of rotation period decay in ...
openaire +2 more sources
Effect of stellar rotation on oscillation frequencies [PDF]
Astrophysics and Space Science, 2010 We investigate whether the rotational splittings of β Cephei stars can give some clue about the existence of a differential rotation in latitude, and if they are contaminated by the cubic order effects of rotation on oscillation frequencies. We also study some properties of splitting asymmetries and axisymmetric mode frequencies which provide seismic ...
Ouazzani, Rhita-Maria +3 more
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Diffusion‐based size determination of solute particles: a method adapted for postsynaptic proteins
FEBS Open Bio, EarlyView.We present a diffusion‐based approach for measuring the size of macromolecules and their complexes, and demonstrate its use on postsynaptic proteins. The method requires fluorescein‐labelled protein samples, a microfluidic device that maintains laminar flow for said samples, a microscope recording the emitted fluorescent signals, and an analytic ...
András László Szabó +7 more
wiley +1 more source
Toward a Self-consistent Hydrodynamical Model of the Solar Tachocline
The Astrophysical JournalThe solar tachocline is a thin internal boundary layer in the Sun located between the differentially rotating convection zone and the uniformly rotating region of the radiative interior beneath. E. A. Spiegel & J. P.
P. Garaud, D. O. Gough, L. I. Matilsky
doaj +1 more source
Living with a Red Dwarf: The Rotation–Age Relationships of M Dwarfs
The Astrophysical Journal Letters, 2023 Age is a fundamental stellar property, yet for many stars, it is difficult to reliably determine. For M dwarfs, it has been notoriously so. Due to their lower masses, core hydrogen fusion proceeds at a much slower rate in M dwarfs than it does in more ...
Scott G. Engle, Edward F. Guinan
doaj +1 more source
A SYSTEMATIC STUDY OF EFFECTS OF STELLAR ROTATION, AGE SPREAD, AND BINARIES ON COLOR–MAGNITUDE DIAGRAMS WITH EXTENDED MAIN-SEQUENCE TURNOFFS [PDF]
, 2016 Stellar rotation, age spread, and binary stars are thought to be the three most possible causes of the peculiar color–magnitude diagrams (CMDs) of some star clusters, which exhibit extended main-sequence turnoffs (eMSTOs).
Zhongmu Li +4 more
semanticscholar +1 more source
Observational studies of stellar rotation [PDF]
EAS Publications Series, 2013 This course reviews the rotational properties of non-degenerate stars as observed from the protostellar stage to the end of the main sequence. It includes an introduction to the various observational techniques used to measure stellar rotation. Angular momentum evolution models developed over the mass range from the substellar domain to high-mass stars
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Constraining Stellar Rotation at the ZAMS
, 2021 As Solar-type stars approach the main sequence, they contract and spin more rapidly; once they reach the main sequence, they stop contracting and their spin speed decreases. This spin-down is thought to be caused by angular momentum lost via stellar winds, but there are currently limited constraints on model behavior at this critical age.
Douglas, Stephanie T. +7 more
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