Flux

Simulations of prominence eruption preceded with large amplitude longitudinal oscillations and draining

Graphic depicting prominence-forming twisted coronal flux rope
Friday, November 6, 2020

We present magnetohydrodynamic (MHD) simulations of the evolution from quasi-equilibrium to eruption of a prominence-forming twisted coronal flux rope under a coronal streamer. The prominence condensations form at the dips of the twisted flux rope due to run-away radiative cooling.

Bhishek Manek

Bhishek Manek is a visiting scientist in the High Altitude Observatory (HAO) at the National Center for Atmospheric Research (NCAR). Bhishek is from the Applied Mathematics department at the University of California Santa Cruz (UCSC), where he is a Ph.D. candidate under the supervision of Prof.

Simulation of Prompt Acceleration of Radiation Belt Electrons during the 16 July 2017 storm

Graph depicting a comparison of simulated and measured fluxes
Wednesday, December 11, 2019

Patel et al. observe that when an interplanetary shock launched from the Sun arrives at Earth, it compresses the dayside magnetic field and an impulse in electric and magnetic field propagates as a characteristic wave mode inside the magnetosphere toward the nightside.

The eruption of a prominence carrying coronal flux rope forward synthesis of the magnetic field strength measurement by COSMOS

(a) The inferred line-of-sight (LOS) magnetic field B_LOS obtained from the forward synthesis of the circular polarization signal from the MHD model data at a time during the quasi-static phase of the flux rope; (b) The same as (a) but only show the pixels of the measured B_LOS with sufficient signal to noise ratio; (c) The axial field strength in the mid cross-section of the flux rope; (d) The 3D field lines of the coronal magnetic field as view
Tuesday, November 13, 2018

From a magnetohydrodynamic (MHD) simulation of the eruption of a prominence hosting coronal flux rope, Yuhong Fan and others carry out forward synthesis of the circular polarization signal (Stokes V signal) of the FeXIII emission line at 1074.7 nm produced by the MHD model.

Variability and predictability of the space environment as related to lower atmosphere forcing

Monthly mean, globally integrated total gravity wave flux of energy
Tuesday, April 4, 2017

Most of the large events affecting the thermosphere and ionosphere part of the space environment come from the Sun, the solar wind, and Earth’s magnetosphere, but even in “quiet time” periods lacking those sources of variability, conditions in the thermosphere and ionosphere continue to fluctuate

CME Initiation, Evolution, and Interplanetary Consequences

HAO scientists have carried out 3D isothermal MHD simulations of the evolution of the large scale coronal magnetic field as a twisted magnetic flux tube is driven (slowly) through the lower boundary into a pre-existing coronal arcade field.

Lisa Upton, A Scientific Dynamo!

Lisa Upton

Lisa is a Visiting Scientist at HAO and also is currently working for Space Systems Research Corporation. In the spring of 2017, Lisa will begin a NSF postdoctoral fellowship at HAO, working as a collaborator with the dynamo group.

Slow appearance of sunspots challenges theory

HAO along with researchers from the Max Planck Institute for Solar System Research, The University of Göttingen, and NorthWest Research Associates have now shown that magnetic flux concentrations forming active regions on the sun emerge at a rate much slower than predicted by the prevailing curre

Convection in Oblate Solar-Type Stars

3D simulation image
Wednesday, July 13, 2016

We present the first global 3D simulations of thermal convection in the oblate envelopes of rapidly-rotating solar-type stars.

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