A Note On Heat Transfer In The Upper Chromosphere And Corona

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Dynamics of the solar atmosphere: Spicules and fibrils - UNH

by AC Sterling 1988 The flow of coronal heat down Into the upper chromosphere is Beckers (1972) notes that spicules near the solar poles seem to follow the polar (coronal) 

The solar atmosphere - Solar Physics and Space Weather

by SK SOLANKI 2001 Cited by 6 associated heating of the chromosphere and corona. In the following we discuss the various rapidly that viscosity and thermal conduction convert the.

Thermal instability and non-equilibrium in solar coronal loops

by P Antolin 2019 Cited by 25 The energy is mostly transferred down to the transition region and upper chromosphere, where it is radiated away and also heats up the 


by JW Reep 2016 Cited by 61 wave numbers, the waves dissipate significantly in the upper chromosphere, strongly heating balance between different types of coronal energy transport.


by GH Fisher 1985 After heating commences at t=0 [s], the upper portion of the corona mechanisms in the chromosphere for thermal model heating seem to be.

the temperature distribution in the solar chromosphere - NASA

oped by Kuperus and Athay (1967), in which thermal conduction downward through the chromosphere- corona transition region is the source of energy that 

Dissipation of Magnetohydrodynamic Waves in the Upper

by GB Laing 1996 Cited by 1 by the dissipation mechanisms of ion viscosity, electron thermal conduction and radiation in an optically thin atmosphere. An overview of coronal features 

Semi-empirical Modeling of the Photosphere, Chromosphere

by JM Fontenla 2016 Cited by 56 structure of the star's chromosphere, chromosphere-corona transition results from the very high thermal conductivity of coronal plasma.

The synthetic chromosphere - DiVA

by JP Bjørgen 2019 losses are much higher in the chromosphere than in the corona. losses in the chromosphere and the corona, and heat conduction along.

Redalyc.Numerical simulation of the cooling of a solar flare

by CAM Briceño 2004 Cited by 2 by including the upper chromosphere in their calculations, and they obtained cooling times including radiative cooling and heating, thermal conduction,.


by GL Withbroe 1983 Cited by 2 fall of spicular material can supply the thermal energy required for heating the upper chromosphere, transition region and possibly corona.

Heating the solar corona by plasma loops - Astronomy

by JMA Ashbourn 2006 Cited by 2 Under certain conditions heat can flow across magnetic fields up temperature gradients, temperature in the upper chromosphere, e.g. hotter than about 5×.7 pages

Observations from Hinode/EIS of intensity oscillations above a

by AK Srivastava 2010 Cited by 24 This may allow the transfer of ∼5.0-min acoustic oscil- lations from the upper chromosphere/TR into the corona. We find that intensity oscillations.

The Environments of the Sun and the Stars - NET

Photosphere Upper chromosphere Lower corona. Corona Note that at a given altitude the parameter may vary by more than two orders of magnitude,.

Solar corona

Energy flux to heat chromosphere: 107 erg cm-2 s-1. ≈ 10 x average energy flux for corona (105 x higher density in chromosphere).


20 Apr 2007 solar transition region or upper chromosphere. The point is that the heat generation does not occur in the corona per se, but rather.

Observations of ubiquitous compressive waves in the - Nature

by RJ Morton 2012 Cited by 145 energy with the potential to meet chromospheric and coronal heating for example, compressive viscosity and thermal conduction15.

The Properties of the Solar Corona and Its Connection to the

by SR Cranmer 2018 Cited by 41 took note of the fact that the solar flare observed in September 1859 was In the upper chromosphere and low corona, heat conduction also 

MHD turbulence and heating of the open field-line solar corona

by WH Matthaeus 2003 Cited by 24 heating the low chromosphere, while waves with P ≈ 300 s heat the upper chromosphere. Hydrodynamic theory provides a satisfactory 

The Solar Corona at Totality - Federation Of American Scientists

urements of solar wind flow, interpreted the steep temperature rise in the chromosphere-corona transition region is uncertain,.

Mapping solar magnetic fields from the photosphere to the

by R Ishikawa 2021 Cited by 2 thermal energy needed to heat the corona must propagate through the chromosphere, explains why it is indeed a crucial interface re-.

Transition Region, Corona, and Solar Wind in Coronal Holes

by JV HOLLWEG 1986 Cited by 406 and chromosphere-corona transition region, the solar wind is viscous and heat conduction damping of sound waves. Coronal holes, however 

njit-etd2016-044 - archives.njit.edu

Printing note: If you do not wish to print this page, then select in the upper solar chromosphere or lower corona, providing the information in the.

Simulating waves in the upper solar atmosphere - CSCAMM

Waves and oscillations are a significant means for the transport and circulation We need to model the conditions in the chromosphere and corona and use 

1 Stellar winds and magnetic fields - silo.tips

of the chromosphere, corona, and solar wind as a unified system. parameters ρ0 and T0 at the coronal base; thermal conduction is not capable 

The Solar Atmosphere - UiO

Looking at the solar photosphere, we see the top of the convection zone in the The magnitude of the magnetic field in the chromosphere (and corona) can.


by H Iijima 2015 Cited by 16 the chromosphere and the corona, and thermal conduction along the the coronal temperature is higher (similar to that in active regions).

Evidence of Non-Thermal Particles in Coronal Loops Heated

by P Testa 2014 Cited by 102 incompatible with heating transported by thermal conduction or by of from the chromosphere to the upper TR, are more tightly coupled as 


Detection of EUV Polar Coronal Holes During Solar Cycle 23. Solar Physics, 257, 99 energy as heat, the chromosphere responds by expanding and send-.

Structures in the outer solar atmosphere - University of Glasgow

by L Fletcher 2014 Cited by 12 thermal conduction from the corona to the lower atmosphere, optically thin radiation to space and mass flows between the upper chromosphere, TR and corona.


velocity, heat conduction is applied only to the electrons, owing to their much higher thermal velocity. Note that. AWSoM also works for three temperatures 

Evidence of ubiquitous Alfvén pulses transporting energy from

by J Liu 2019 Cited by 14 waves might transport enough energy from the photosphere to heat up the local chromo- than enough to balance the local upper chromospheric energy.

Abstract Book - Indian Institute of Astrophysics

1 Mar 2021 However, recent studies of the p-modes in the upper chromosphere have also revealed significant power enough to heat the solar corona.


by JA Klimchuk 2014 Cited by 40 occur in the upper chromosphere rather than in the corona (Hansteen et al. 2010). The plasma is heated directly rather than by a thermal conduction flux.

Kinetic Physics of the Solar Corona and Solar Wind

by E Marsch Cited by 650 3.4 The failure to heat chromosphere or corona by collisions Figure 1 shows in the upper frame a typical solar wind electron VDF 


by RL Moore 1978 phase all flare emission from chromospheric through coronal temperature levels may well be supplied by heat transfer from the thermal X-ray plasma.

Astrophysics The emergence of magnetic flux - Warwick WRAP

twisted flux tube is inserted into the upper part of the convec- tion zone which rises by sphere/chromosphere, isothermal corona and a transition re- gion between the senting no heat transfer), a Joule heating term from ion-electron collisions, and Note that due to the anisotropic nature of the dissipation mechanism, i.e. 

Coronal heating, densities, and temperatures and solar wind

1 Nov 1995 The corona loses energy through heat conduction into lect at the top of the chromosphere until the density at the.

Numerical Study of Coronal Mass Ejections, Shocks, and

by M Jin 2014 left), proton temperature (top right), radial solar wind velocity (bot- less heat conduction, we simulate CME propagation from the chromosphere to 1 AU.

Stellar Chromospheres - Exoplanets - Yale University

25 Jan 2016 Upper Chromosphere: Above the temperature minimum where Corona: Extended region of high ionization where thermal gradients.

JAKO198508658292634.pdf - Korea Science

by MG Lee 1985 Cited by 4 with a period of about 20 second can heat the low umbral chromospheres which is as much as the radiative loss from the umbral chromosphere and corona.

The role of partial ionization effects in the chromosphere

by J Martínez-Sykora 2015 Cited by 29 The proponents note that mass flux also can contribute to transport or (f) in the upper chromosphere, transition region and corona, the thermal 

Physics of the chromosphere and the lower coronal boundary

modulates flow of mass, momentum, energy and magnetic field into the corona photosphere. - forced top of chromosphere, corona. - force free 


by H PETER 2002 Cited by 3 photosphere to the corona according to the first ionisation potential, for our interpretation of the structure of the solar atmosphere and a note to 


by S Kamio 2005 Cited by 23 Note that CDS cannot determine absolute velocities, so perature ranges of the upper chromosphere, transition region, and low corona.

The Challenge of Chromospheric Physics - JSTOR

by RG Athay 1964 Cited by 7 corona. The great brilliance of the photosphere obscures the chromosphere Spicules in the upper and middle chromosphere, as observed in the Ha line of 

Aerodynamic phenomena in stellar atmospheres, a bibliography

A Note on Heat Transfer in the Upper Chromosphere and Corona; Giovanelli,. R.G.; M.N. ,. 109, 372, 1949. Conduction along lines of force of general magnetic 

Magnetohydrodynamic and thermal processes in solar flare

by W Tend Cited by 3 upper solar atmosphere that converts from 102^ ergs up to chromosphere-corona transition region could well be in a continual state of motion, 

Title Nonlinear Alfvén Wave Model for Solar/Stellar

by T Sakaue 2021 2 Energy Transfer by Nonlinear Alfvén Waves in the Solar Chromosphere, and Its Effect on Spicule Dynamics, Coronal Heating, and Solar Wind 

Lecture 7: From the Photosphere to the Hot Corona

the upper chromosphere is much hotter, there must be a temperature minimum are assumed then losses due to radiation and heat conduction can be