Plasma Beta above a Solar Active Region: Rethinking the Paradigm

By G. A. Gary. 2001

433 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/d91712939c7b7188ffc0faf155c0e2f89c7ec688

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

Waves in the Magnetized Solar Atmosphere. II. Waves from Localized Sources in Magnetic Flux Concentrations (2003, background): “The best advice one can give is to be aware of the regions surrounding the place where the observations are obtained (Gary 2001; McIntosh et al. 2001; McIntosh & Judge 2001).”
Band-splitting of coronal and interplanetary type II bursts - III. Physical conditions in the upper corona and interplanetary space (2004, methodology): “However, in the corona the value of β increases with the height (cf. Gary 2001, see also 4 The low v∗ values are probably not due to errors in measurements: solar wind is inhomogeneous, so the density and the plasma speed can locally depart significantly from the “average” wind characteristics.”
The magnetic field in the solar atmosphere (2014, background): “Gary (2001) was able to confirm that finding by combining a plasma pressure and magnetic field model to estimate the pattern of interchanging dominance of plasma and magnetic pressure with height in the solar atmosphere (see Figure 5).”
Solar Force-free Magnetic Fields (2012, methodology): “The pseudo-current method developed by Gary and Démoulin (1995) uses as the initial step the potential-field acute angle method and subsequently applies this result to compute an approximation for the vertical electric current density.”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, result): “The total magnetic field expansion from y = 600 km upwards in this model is a factor of 5, similar to that suggested by Gary (2001).”
Particle acceleration and kinematics in solar flares – A Synthesis of Recent Observations and Theoretical Concepts (Invited Review) (2002, background): “On the other side, the observed long duration of hot cusps might not be consistent with fast reconnection and could be interpreted alternatively (e.g. by upward diffusion of hot plasma in a high-β environment, see Gary 2001).”
Band-splitting of coronal and interplanetary type II bursts - II. Coronal magnetic field and Alfvén velocity (2002, background): “Highly structured patterns observed in the EUV wavelength range indicate that the coronal plasma is controlled by the magnetic field, i.e., β 1 (for a discussion see Gary 2001).”
Hot coronal loop oscillations observed with SUMER: Examples and statistics (2003, background): “However, Gary (2001) argued that the plasma β can increase beyond unity at relatively low coronal heights (h ∼ 14 − 3 4 R ).”
Nonlinear Force-Free Modeling of Coronal Magnetic Fields Part I: A Quantitative Comparison of Methods (2006, background): “The coronal field is therefore often said to be “forcefree,” i.e., free of forces other than the balancing electromagnetic forces that it exerts on itself (but see, e.g., Gary, 2001).”
Preprocessing of Vector Magnetograph Data for a Nonlinear Force-Free Magnetic Field Reconstruction (2006, background): “…extrapolations, vector magnetogram, SFT Abbreviations: KAP – Kluwer Academic Publishers; compuscript – Electronically submitted article JEL codes: D24, L60, 047 Nomenclature: KAP – Kluwer Academic Publishers; compuscript – Electronically submitted article Solar Physics, Vol. 233, 215-232 (2006)”
The Origin, Early Evolution and Predictability of Solar Eruptions (2018, background): “…CME rapidly decreases with distance from the Sun, because both the electric current I and the magnetic field B protruding through the magnetic structure decrease (for the dependence of the magnetic field on height see, e.g., Dulk and McLean, 1978; Gary, 2001; Vršnak et al, 2002, 2004a; Liu, 2008).”
A CRITICAL ASSESSMENT OF NONLINEAR FORCE-FREE FIELD MODELING OF THE SOLAR CORONA FOR ACTIVE REGION 10953 (2009, background): “The most conspicuous reason is that the photospheric layers of the Sun, from which originate the Hinode/SOT-SP magnetogram data used here, do contain Lorentz, buoyancy, and pressure gradient forces and thus are not force-free to begin with (Metcalf et al. 1995; Gary 2001).”
Optimization code with weighting function for the reconstruction of coronal magnetic fields (2008, background): “It is generally assumed that the magnetic pressure in the corona is much higher than the plasma pressure (small plasma β) and that therefore the magnetic field is nearly force-free (for a critical view of this assumption see (Gary, 2001)).”
Evidence of EIT and Moreton Waves in Numerical Simulations (2002, background): “Such a largeb is possible in the middle corona but unrealistic in the low corona (e.g., Gary 2001).”
Interaction of EIT Waves with Coronal Active Regions (2001, result): “Because of the bipolar structure of the active region magnetic field, the value of varies slowly between the poles and increases away from the poles, to values of order unity, consistent with the values found by Gary (2001).”