Homology tutorial Hugh Hudson Solar MURI 21-Nov-03.

Slides:



Advertisements
Similar presentations
Masuda Flare: Remaining Problems on the Looptop Impulsive Hard X-ray Source in Solar Flares Satoshi Masuda (STEL, Nagoya Univ.)
Advertisements

Observations on Current Sheet and Magnetic Reconnection in Solar Flares Haimin Wang and Jiong Qiu BBSO/NJIT.
The magnetic nature of solar flares Paper by E.R. Priest & T.G. Forbes Review presented by Hui Song.
R. P. Lin Physics Dept & Space Sciences Laboratory University of California, Berkeley The Solar System: A Laboratory for the Study of the Physics of Particle.
Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
Active Region Evolution and the Removal of Magnetic Helicity by CMEs Len Culhane Mullard Space Science Laboratory University College London.
STEREO AND SPACE WEATHER Variable conditions in space that can have adverse effects on human life and society Space Weather: Variable conditions in space.
Hard X-rays associated with CMEs H.S. Hudson, UCB & SPRC Y10, Jan. 24, 2001.
Coronal Loop Oscillations and Flare Shock Waves H. S. Hudson (UCB/SSL) & A. Warmuth (Astrophysical Institute Potsdam) Coronal loop oscillations: introduction.
24 Oct 2001 A Cool, Dense Flare T. S. Bastian 1, G. Fleishman 1,2, D. E. Gary 3 1 National Radio Astronomy Observatory 2 Ioffe Institute for Physics and.
East-West Asymmetry of the Yohkoh Soft X-ray Corona L.W. Acton 1, D.E. McKenzie 1, A. Takeda 1, B.T. Welsch 2,and H.S. Hudson 2,3 1 Montana State University,
SHINE Campaign Event: 1-2 May 1998 Brian Welsch (& Yan Li) Space Sciences Laboratory, UC Berkeley Introduction: Data, Context, etc. Work: Completed & Ongoing.
Intense Flares Without Solar Energetic Particle Events N. V. Nitta (LMSAL), E. W. Cliver (AFRL), H. S. Hudson (UCB) Abstract: We study favorably located.
Solar evidence for magnetic reconnection H. S. Hudson Space Sciences Lab, UC Berkeley.
Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions ITP Santa Barbara, Jan. 18, 2002Hugh.
MRT workshop, August 10, 2004 Active-region magnetic structures and their perturbations by flares H.S. Hudson SSL/UCB.
Uses of solar hard X-rays Basics of observations Hard X-rays at flare onset The event of April 18, 2001 Conclusions Yohkoh 10th Jan. 21, 2002Hugh Hudson,
CAWSES December 10, CMEs H.S. Hudson Space Sciences Lab, UC Berkeley.
Coronal hard X-rays prior to RHESSI H. S. Hudson Space Sciences Lab, UC Berkeley.
White-Light Flares and HESSI Prospects H. S. Hudson (UCB and SPRC) March 8, 2002.
“Refinements to flare energy estimates…” Emslie et al., et Hugh too, JGR 110, 2005 Particles Flows Waves Corona B 2 /8  EM radiation Mechanical energy.
RHESSI OBSERVATIONS OF FLARE FOOTPOINTS AND RIBBONS H. Hudson and M. Fivian (SSL/UCB)
The hard X-ray spectral structure of flare ribbons H. Hudson, L. Fletcher, S. Krucker, J. Pollock.
SEPs and Solar Radio Bursts S. Krucker and H. Hudson Time-of-flight analysis of SEP propagation Connectivity of the SEP field lines SIRA relevance.
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.
Reconstructing Active Region Thermodynamics Loraine Lundquist Joint MURI Meeting Dec. 5, 2002.
The Yohkoh observations of solar flares Hugh Hudson UCB.
Stanford, January Solar flares, magnetars, and helioseismology H.S. Hudson SSL/UCB.
Homologous large-scale activity in the solar eruptive events of November 24–26, 2000 I. M. Chertok a, V. V. Grechnev b, H. S. Hudson c, and N.V. Nitta.
Ward Manchester University of Michigan Coupling of the Coronal and Subphotospheric Magnetic Field in Active Regions by Shear Flows Driven by The Lorentz.
The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.
Kathy Reeves Harvard-Smithsonian Center for Astrophysics Terry Forbes University of New Hampshire Partitioning of energy in a loss-of-equilibrium CME model.
IGPP, March Coronal shock waves observed in images H.S. Hudson SSL/UCB.
Glasgow, March 24, 2005 Large-scale coronal shock waves H.S. Hudson SSL/UCB.
Coronal Loop Oscillations and Flare Shock Waves H. S. Hudson (UCB/SSL) & A. Warmuth (Astrophysical Institute Potsdam) Coronal loop oscillations: (Fig.
On the Origin of Strong Gradients in Photospheric Magnetic Fields Brian Welsch and Yan Li Space Sciences Lab, UC-Berkeley, 7 Gauss Way, Berkeley, CA ,
Late-phase hard X-ray emission from flares The prototype event (right): March 30, 1969 (Frost & Dennis, 1971), a very bright over-the-limb event with a.
Free Magnetic Energy in Solar Active Regions above the Minimum-Energy Relaxed State (Regnier, S., Priest, E.R ApJ) Use magnetic field extrapolations.
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.
Coronal hard X-rays prior to RHESSI H. S. Hudson Space Sciences Lab, UC Berkeley.
V.I. Abramenko, V.B. Yurchyshyn, H. Wang, T.R. Spirock, P.R. Goode Big Bear Solar Observatory, NJIT Crimean Astrophysical Observatory, Ukraine
Coronal holes as seen in soft X-rays H. S. Hudson (UCB and SPRC) SOHO-11, Davos, March 13, 2002.
Elmau III, March 16, 2004 Coronal mass ejections A critical view of interpretations H.S. Hudson (UC Berkeley)
The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.
CAWSES December 10, CMEs H.S. Hudson 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.
Data-Driven MHD Modeling of CME Events
MAGNETIC TWIST OF EUV CORONAL LOOPS OBSERVED BY TRACE RyunYoung Kwon, Jongchul Chae Astronomy Program, School of Earth and Environmental Science Seoul.
Flares in and their associations with CMEs N.V. Nitta, J.P.Wuelser, M. J. Aschwanden, J. R. Lemen (LMSAL), D. M. Zarro (Adnet, Inc.)
Footpoint behavior Hugh Hudson UCB Galileo science meeting Nobeyama, July 12, 2002.
Coronal hard X-ray sources and associated decimetric/metric radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA) S.R Kane G. Hurford.
Coronal Dynamics - Can we detect MHD shocks and waves by Solar B ? K. Shibata Kwasan Observatory Kyoto University 2003 Feb. 3-5 Solar B ISAS.
Measurement of the Reconnection Rate in Solar Flares H. Isobe 2004/12/6 Taiyo-Zasshikai.
Pre-flare activity of M1.2 flare 김수진 1,2, 문용재 1, 김연한 1, 박영득 1, 김갑성 2 1. Korea Astronomy and Space Science Institute 2. Kyung Hee University.
Current Sheets from WL and UV data: open questions Alessandro Bemporad INAF – Arcetri Astrophysical Observatory 1° ISSI Group Meeting October 23-27, 2006,
SHINE SEP Campaign Events: Detailed comparison of active regions AR9906 and AR0069 in the build-up to the SEP events of 21 Apr 2002 and 24 Aug 2002 D.
KASI Low atmospheric reconnections associated with an eruptive flare Yong-Jae Moon(1), Jongchul Chae(2), Young-Deuk Park(1) 1: Korea Astronomy and.
Katharine K. Reeves 1, Terry G. Forbes 2, Jon Linker 3 & Zoran Mikić 3 1 Harvard-Smithsonian Center for Astrophysics 2 University of New Hampshire 3 Science.
III. APPLICATIONS of RECONNECTION Yohkoh Bright Pts Loops Holes A magnetic world T=few MK 1. Coronal Heating.
ISSI, Beijing, China. The famous example of the decaying kink oscillations of coronal loops observed with the TRACE ISSI, Beijing,
Magnetic Helicity and Solar Eruptions Alexander Nindos Section of Astrogeophysics Physics Department University of Ioannina Ioannina GR Greece.
CME/Flare energetics and RHESSI observations H.S. Hudson SSL/UCB.
Sweet Solar SAP: Boiling Down the Thermal Energy Content of Supra-Arcade Plasma Ashley Armstrong Advisor: Dr. Kathy Reeves Solar REU Summer 2012.
Ward Manchester University of Michigan
The CME-Flare Relationship in Homologous Eruptive Events
Nonthermal Electrons in an Ejecta Associated with a Solar Flare
N. Nitta1, J.-P. Wuelser1, J. Lemen1, M. Aschwanden1, G. Attrill2
Presentation transcript:

Homology tutorial Hugh Hudson Solar MURI 21-Nov-03

Definition: Homology is the tendency for event morphology to repeat precisely. Comment: Here morphology means anything at all: image, time series, spectrum, location…

Trevisan et al., RMA&A 21, 557, 1990 HH

Cliver & Wefer, Solar Phys. 71, 39, 1981 Microwaves

TRACE 24 October :17 24 October :02 K. Schrijver, 20-Nov-03

Yohkoh spiky arcades

Morita et al., Solar Phys. 200, 137, 2001 Yohkoh “candle flame”

Bastille Day?

Processes in which the entropy of an isolated system would decrease do not occur, or, in every process taking place in an isolated system, the entropy of the system either increases or remains constant Second law of thermodynamics Solar application An eruption (e.g., a CME) proceeds irreversibly because Of energy dissipation (e.g., through reconnection or shock waves

Common knowledge Ranns et al., A&A 360, 1173 (2000) Nitta & Hudson, GRL 28, 3801 (2001) Emerging flux leads to near-homology Comment This explanation for homologous flares implies some persistence in the flux emergence, ie a coherence over time scales of the interval of homology

Heyvaerts, Priest & Rust, ApJ 216, 123, 1977 Standard emerging- flux cartoon Note the poor cartoonsmanship - the panels show different field lines

The flow associated with flux emergence implies changes in the footpoint geometry. Successive events would have different coronal null geometries. The separatrix current in this geometry circulates only in the corona.

Nitta & Hudson, GRL 28, 3801 (2001)

Soft X-rays, hard X-rays

Magnetism (MDI), hard X-rays (HXT), soft X-rays (SXT)

Emerging flux time-history

Chertok et al., JGR to be published (2003? 2004?)

Homologous dimmings

Dimmings at various wavelengths

Conclusions Homologous flares might be explainable by persistent flux emergence, even in a reconnection model Homologous CMEs might be explained similarly, if they are basically derived from small spatial scales in ARs Chertok et al dash that hope, though, because the homology extends to the quiet corona on large scales, with dissipation