Momentum Conservation in Flares H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow.

Slides:

Advertisements

Similar presentations

The Science of Solar B Transient phenomena – this aim covers the wide ranges of explosive phenomena observed on the Sun – from small scale flaring in the.

Advertisements

Back Reaction on the Photospheric Magnetic field in Solar Eruptions Dandan Ye.

Flare-Associated Magnetic Field Changes Observed with HMI by Brian T. Welsch & George H. Fisher Space Sciences Lab, UC-Berkeley Permanent changes in photospheric.

HMI OBSERVATIONS OF TRANSIENT PHENOMENA Juan Carlos Martínez Oliveros Space Sciences Laboratory, UC Berkeley Charles Lindsey, Hugh Hudson, S. Couvidat,

The Focusing Optics X-ray Solar Imager (FOXSI) Steven Christe 1, S. Krucker 2, L. Glesener 2, S. Ishikawa 3, B. Ramsey 4, T. Takahashi 3, R.P. Lin 2 1.

The effects of canopy expansion on chromospheric evaporation driven by thermal conductions fronts Authors: F. Rozpedek, S. R. Brannon, D. W. Longcope Credit:

Flare energy and fast electrons via Alfvén waves H. S. Hudson & L. Fletcher SSL/Berkeley and Glasgow U. Predictions for Hinode/SOT flare observations.

Flare energy supply and magnetic field variations H. S. Hudson & B. T. Welsch Space Sciences Lab, UC Berkeley Trying to predict vector field changes during.

Flare footpoints and ribbons: The impulsive phase H.S. Hudson Space Sciences Lab, UC Berkeley.

Flares and global waves, including seismic H. S. Hudson 1, C. A. Lindsey 2, J. Martinez-Oliveros 1 1 Space Sciences Laboratory, University of California,

Flare waves and the impulsive phase H. S. Hudson Space Sciences Laboratory University of California, Berkeley.

Solar and Stellar Flares Hugh S. Hudson SSL, UC Berkeley 1 May

Flare Dynamics in the Lower Solar Atmosphere H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group,

The optical and UV continuum in the impulsive phase H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA.

Flare Dynamics in the Lower Solar Atmosphere H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group,

Flare Dynamics in the Lower Solar Atmosphere H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group,

An Overall Framework for Solar Flares? H. S. Hudson Space Sciences Laboratory University of California, Berkeley CS-16 29/08/10.

Momentum Conservation in Flares H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Canfield 08/09/10.

The mystery of the MISSING MOMENTUM H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow.

Simulation of Flux Emergence from the Convection Zone Fang Fang 1, Ward Manchester IV 1, William Abbett 2 and Bart van der Holst 1 1 Department of Atmospheric,

Flare global waves of three kinds H. S. Hudson 1, C. A. Lindsey 2, J. Martinez-Oliveros 1 1 Space Sciences Laboratory, University of California, Berkeley,

Chromospheric flares in the modern era H. Hudson Space Sciences Lab, UC Berkeley.

Chip Manchester 1, Fang Fang 1, Bart van der Holst 1, Bill Abbett 2 (1)University of Michigan (2)University of California Berkeley Study of Flux Emergence:

Momentum Balance in Eruptive Solar Flares: The Role of the Lorentz Force George H. Fisher, David J. Bercik, Brian T. Welsch, & Hugh S. Hudson Space Sciences.

Flare waves and the impulsive phase H. S. Hudson Space Sciences Laboratory University of California, Berkeley.

Hard X-ray sources in the solar corona H.S. Hudson Space Sciences Lab, UC Berkeley.

Transients in RHESSI and Chromospheric flares H. Hudson Space Sciences Lab, UC Berkeley.

White-Light Flares and HESSI Prospects H. S. Hudson (UCB and SPRC) March 8, 2002.

Chapter 7 The Sun. Solar Prominence – photo by SOHO spacecraft from the Astronomy Picture of the Day site link.

Solar-B XRT XRT-1 The Science and Capability of the Solar-B / X-Ray Telescope Solar-B XRT Presenter: Ed DeLuca Smithsonian Astrophysical Observatory.

Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.

Center for Space Environment Modeling Ward Manchester University of Michigan Yuhong Fan High Altitude Observatory SHINE July.

Flare-related current systems H. S. Hudson & B. T. Welsch Space Sciences Lab, UC Berkeley.

Stanford, January Solar flares, magnetars, and helioseismology H.S. Hudson SSL/UCB.

Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.

IGPP, March Coronal shock waves observed in images H.S. Hudson SSL/UCB.

Hard X-ray Diagnostics of Solar Eruptions H. Hudson SSL, UC Berkeley and U. Of Glasgow.

The nature of impulsive solar energetic particle events N. V. Nitta a, H. S. Hudson b, M. L. Derosa a a Lockheed Martin Solar and Astrophysics Laboratory.

Magnetic Reconnection Rate and Energy Release Rate Jeongwoo Lee 2008 April 1 NJIT/CSTR Seminar Day.

Flare energy and fast electrons via Alfvén waves H. S. Hudson & L. Fletcher SSL/Berkeley and Glasgow U.

Microflares now, major flares soon H.S. Hudson Space Sciences Lab, UC Berkeley.

Flare-related current systems H. S. Hudson & B. T. Welsch Space Sciences Lab, UC Berkeley.

Royal Astronomical Society Oration H. S. Hudson & B. J. Welsch Space Sciences Lab, UC Berkeley.

RHESSI and global models of flares and CMEs: What is the status of the implosion conjecture? H.S. Hudson Space Sciences Lab, UC Berkeley.

SMESE: a French/Chinese Solar “SMEX” H.S. Hudson Space Sciences Lab, UC Berkeley.

Physical analogies between solar chromosphere and earth’s ionosphere Hiroaki Isobe (Kyoto University) Acknowledgements: Y. Miyoshi, Y. Ogawa and participants.

Solar-B/EIS high-cadence observation for diagnostics of the corona and TR S. Kamio (Kyoto Univ.) Solar-B domestic meeting.

Co-spatial White Light and Hard X-ray Flare Footpoints seen above the Solar Limb: RHESSI and HMI observations Säm Krucker Space Sciences Laboratory, UC.

ABSTRACT This work concerns with the analysis and modelling of possible magnetohydrodynamic response of plasma of the solar low atmosphere (upper chromosphere,

Transition Region And Coronal Explorer Observes three-dimensional magnetic structures in the Photosphere Defines the geometry and dynamics of the Transition.

Multiwavelength observations of a partially occulted solar flare Laura Bone, John C.Brown, Lyndsay Fletcher.

Footpoint behavior Hugh Hudson UCB Galileo science meeting Nobeyama, July 12, 2002.

Atmospheric transport and chemistry lecture I.Introduction II.Fundamental concepts in atmospheric dynamics: Brewer-Dobson circulation and waves III.Radiative.

Coronal hard X-ray sources and associated decimetric/metric radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA) S.R Kane G. Hurford.

_________________at the centre of our solar system.

El Caracol - Ancient Mayan Observatory El Castillo.

Solar and STP science with AstroGrid Silvia Dalla School of Physics & Astronomy, University of Manchester A PPARC funded project.

1 Introduction: Onset of solar flares and coronal mass ejections Yokoyama, T. Dept. Earth & Planetary Science, University of Tokyo Isobe, H. Univ. Tokyo.

ALFVEN WAVE ENERGY TRANSPORT IN SOLAR FLARES Lyndsay Fletcher University of Glasgow, UK. RAS Discussion Meeting, 8 Jan

Energy Budgets of Flare/CME Events John Raymond, J.-Y. Li, A. Ciaravella, G. Holman, J. Lin Jiong Qiu will discuss the Magnetic Field Fundamental, but.

Flare Ribbon Expansion and Energy Release Ayumi ASAI Kwasan and Hida Observatories, Kyoto University Explosive Phenomena in Magnetized Plasma – New Development.

Sun Notes. Characteristics CLOSEST star to earth CLOSEST star to earth The bright star in the center is Proxima Centauri.

Global Forces in Eruptive Solar Flares: The Role of the Lorentz Force George H. Fisher, Benjamin J. Lynch, David J. Bercik, Brian T. Welsch, & Hugh S.

Shock heating by Fast/Slow MHD waves along plasma loops

Observations –Morphology –Quantitative properties Underlying Physics –Aly-Sturrock limit Present Theories/Models Coronal Mass Ejections (CME) S. K. Antiochos,

CME/Flare energetics and RHESSI observations H.S. Hudson SSL/UCB.

Relationships Between Flares and CME’s Monday, 23 June 2008 Monday, 23 June, 1:30pm, Grindelwald, we have 3 Invited speakers, plenty of extra time for.

Flare footpoints in optical and UV Lyndsay Fletcher University of Glasgow RHESSI 10, August 4 th 2010, Annapolis TRACE WL ~2s time cadence, 0.5” pixel.

Phillip Chamberlin Solar Flares (303) University of Colorado

The Sun: Our Star.

Presentation transcript:

Momentum Conservation in Flares H. S. Hudson Space Sciences Laboratory, University of California, Berkeley, USA Astronomy & Astrophysics Group, Glasgow Colleagues George Fisher, Lyndsay Fletcher, Bill Abbett, Alex Russell Warwick Nov. 19, 2010

History of flare momentum studies “The importance of particle beam momentum in beam-heated models of solar flares,” Brown & Craig 1984 (14 citations) “The unimportance of beam momentum in electron- heated models of solar flares,” McClymont & Canfield, 1984 (12 citations) “Momentum balance in four solar flares,” Canfield et al., 1990 (49 citations) Warwick Nov. 19, 2010

Four Impulses Primary energy release in the corona (CME?) Chromospheric heating: evaporation and downward shock (Kostiuk & Pikel’ner 1974) Interruption of evaporative flow (new idea 1997) “Coronal rain” from cooling loops Warwick Nov. 19, 2010

Seismic Waves (“sunquakes”) Seismic wave: example of 28-Oct-03 multiple radiant points HXR association now many examples (Kosovichev 2007) Acoustic source: holographic imaging WLF (left) matches source “egression power” (right) easier to see in umbra (Source Lindsey & Donea 2008)

Warwick Nov. 19, 2010 Representative Parameters

Momentum conservation in primary energy release Warwick Nov. 19, 2010 Energy source Recoil Impulse on Photosphere Low-  loop

Warwick Nov. 19, 2010 Momentum cartoon 1 1 Simplified view of vertical component

Warwick Nov. 19, 2010 Momentum estimates 1 1 Scaled to X1

Warwick Nov. 19, 2010 Inferences about momentum There is sufficient momentum in the coronal energy flux to explain the seismic wave CME acceleration predicts one photospheric impulse; evaporation two of opposite signs We don’t know which particular mechanism couples best into the sunquake yet

Warwick Nov. 19, 2010 Time scales Fontenla (2009) umbra model 3000 G Pulse at 600 km

Speculations Analysis of momentum transfer should help in understanding sunquakes (Shock? Backwarming? Lorentz force?) The initial flare energy release and coupling into CME flows, if any, require wave concepts (ExB/v A ) There are several immediate problems worth analysis (imho) Warwick Nov. 19,

Backup slides Warwick Nov. 19, 2010

Flare energy Woods et al 2004 Hudson et al 2006 Short-lived Small-scale 1 1 TRACE 0.5” pixels

Warwick Nov. 19, 2010 The Lorentz force in context “…an enormous amount of magnetic energy…seems to be annihilated during the flare. This should cause a subsequent relaxation of the entire field structure…moving large masses…” - Wolff 1972 “The magnetic force applied to the photosphere…1.2 x dyne…” - Anwar et al (McClymont) “Magnetic forces should be of particular significance… where the magnetic field is significantly inclined from vertical.” - Donea & Lindsey 2005 “Our estimates suggest that the work done by Lorentz forces in this back reaction could supply enough energy to explain observations of flare-driven seismic waves.” - Hudson et al (“Jerk”)

Warwick Nov. 19, 2010 Magnetic changes during flares “Confusogram” legend: 10x10 2.5” pixels 240 minutes time base 500 G magnetic range (Sudol & Harvey 2005)

Warwick Nov. 19, 2010 Significance of low β In the active-region corona, except possibly for small inclusions, β is low. Thus gas pressure is explicitly unimportant. At low β all visible structures are mere tracers and can’t be dynamically important. This also applies to the sunspot regions where seismic waves are launched.