Results 41 to 50 of about 3,389 (211)
Stellar dynamics: Rotation, convection, and magnetic fields [PDF]
, 2015 Stars are changing entities in a constant evolution during their lives. At non-secular time scales (from seconds to years) the effect of dynamical processes such as convection, rotation, and magnetic fields can modify the stellar oscillations. Convection excites acoustic modes in solar-like stars, while rotation and magnetic fields can perturb the ...
Mathur, S., Ballot, J., Garcia, R. A.
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Optimizing photoexcitation conditions for time‐resolved X‐ray solution scattering experiments
FEBS Open Bio, EarlyView.Time‐resolved X‐ray solution scattering (TR‐XSS) is a powerful technique to visualize how proteins change their structure in real time after light activation. Selecting the right laser photoexcitation conditions—fluence, excitation geometry, and sample refresh rate—is critical to maximize the experimental signal while avoiding unwanted side effects ...
Matteo Levantino
wiley +1 more source
Magnetic Fields on Solar-Type Stars: The Solar-Stellar Connection [PDF]
, 2016 Our understanding of solar magnetic fields is significantly more detailed than we can achieve for other stars. However, over the last few decades, techniques such as Zeeman Doppler Imaging (ZDI), have delivered major advances in the study of stellar ...
Marsden, Stephen (5124401) +1 more
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Relationships Between Solar and Stellar Magnetic Fields [PDF]
Symposium - International Astronomical Union, 1983 Observational and theoretical studies of solar and stellar magnetic fields are reviewed. The discussion draws together several themes that emerged during IAU Symposium 102 on “Solar and Stellar Magnetic Fields: Origins and Coronal Effects,” and identifies a number of areas in which research over the next few years is likely to be fruitful.
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Adenosine triphosphate as a modulator of protein interactions and stability
FEBS Open Bio, EarlyView.ATP is best known as the cell's energy currency, but it also shapes how proteins fold, interact, aggregate and form biomolecular condensates. This review explains the emerging physical principles behind these effects, including weak binding to charged protein regions, magnesium‐dependent behaviour and concentration‐dependent control of protein ...
Shuyuan Tan, Robin Curtis
wiley +1 more source
Development and application of a global magnetic field evolution model for the solar corona [PDF]
, 2009 Magnetic fields are fundamental to the structure and dynamics of the Sun’s corona. Observations show them to be locally complex, with highly sheared and twisted fields visible in solar filaments/prominences.
Yeates, Anthony Robinson
core
Early Stellar Evolution and the Role of Magnetic Fields [PDF]
, 2017 <p>Presentation given at the 2017 Georgia Regional Astronomy Meeting (GRAM) at the University of Georgia (Athens, GA, USA).</p> <p><strong>Abstract</strong><br> Young low-mass stars often exhibit observational ...
Feiden, Gregory A. (5304169) +1 more
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FEBS Open Bio, EarlyView.We describe detailed protocols for the purification and preparation of Marchantia polymorpha Auxin Response Factor 2 (MpARF2). This protein is fused to an MBP solubility tag and an mNG fluorescent tag and is purified from Escherichia coli. The presented procedures make it possible to study MpARF2 assemblies, which could arise from phase separation ...
Bas Janssen +5 more
wiley +1 more source
Laboratory astrophysics : investigation of planetary and astrophysical maser emission [PDF]
, 2013 This paper describes a model for cyclotron maser emission applicable to planetary auroral radio emission, the stars UV Ceti and CU Virginus, blazar jets and astrophysical shocks.
Ronald K +27 more
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Modelling stellar coronal magnetic fields [PDF]
Proceedings of the International Astronomical Union, 2010 AbstractOur understanding of the structure and dynamics of stellar coronae has changed dramatically with the availability of surface maps of both star spots and also magnetic field vectors. Magnetic field extrapolations from these surface maps reveal surprising coronal structures for stars whose masses and hence internal structures and dynamo modes may
Jardine, Moira +3 more
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