Interaction between emerging flux and large scale loop systems observed with Hinode XRT Abstract Hinode XRT reveals ubiquitous large-scale connections.

Slides:



Advertisements
Similar presentations
RHESSI observations of LDE flares – extremely long persisting HXR sources Mrozek, T., Kołomański, S., Bąk-Stęślicka, U. Astronomical Institute University.
Advertisements

Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team.
Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
Coronal Responses to Explosive Events Adria C. Updike Smith College / Harvard-Smithsonian Center for Astrophysics Amy Winebarger and Kathy Reeves, Center.
Study of Magnetic Helicity Injection in the Active Region NOAA Associated with the X-class Flare of 2011 February 15 Sung-Hong Park 1, K. Cho 1,
Jan 13, 2009ISSI1 Modeling Coronal Flux Ropes A. A. van Ballegooijen Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, U.S.A Collaborators:
A Multi-Wavelength View of an Active Region Structure around a Filament Channel L. Lundquist, 1 K. Reeves, 1 A. van Ballegooijen, 1 T. Sakao, 2 and the.
Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003.
Anti-parallel versus Component Reconnection at the Magnetopause K.J. Trattner Lockheed Martin Advanced Technology Center Palo Alto, CA, USA and the Polar/TIMAS,
Modeling the Magnetic Field Evolution of the December Eruptive Flare Yuhong Fan High Altitude Observatory, National Center for Atmospheric Research.
Intense Flares Without Solar Energetic Particle Events N. V. Nitta (LMSAL), E. W. Cliver (AFRL), H. S. Hudson (UCB) Abstract: We study favorably located.
SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no.]1 I: C1/M8/C10 Transients: Drivers & Destabilization.
Vincent Surges Advisors: Yingna Su Aad van Ballegooijen Observations and Magnetic Field Modeling of a flare/CME event on 2010 April 8.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
Valentina Abramenko Big Bear Solar Observatory of NJIT Multi-fractality of Solar Magnetic Fields: New Progress with HMI Abstract. The SDO/HMI instrument.
Solar Polar Field Observed by SOHO/MDI and Hinode Yang Liu Stanford University 10/01/ Hinode Workshop.
Nonlinear Force Free Field Models for AR J.McTiernan, H.Hudson (SSL/UCB) T.Metcalf (LMSAL)
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.
Identifying and Modeling Coronal Holes Observed by SDO/AIA, STEREO /A and B Using HMI Synchronic Frames X. P. Zhao, J. T. Hoeksema, Y. Liu, P. H. Scherrer.
Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.
The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.
Flares and Eruptive Events Observed with the XRT on Hinode Kathy Reeves Harvard-Smithsonian Center for Astrophysics.
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 ,
Helicity as a Component of Filament Formation D.H. Mackay University of St. Andrews Solar Theory Group.
Study of magnetic helicity in solar active regions: For a better understanding of solar flares Sung-Hong Park Center for Solar-Terrestrial Research New.
Center for Space Environment Modeling W. Manchester 1, I. Roussev, I.V. Sokolov 1, 1 University of Michigan AGU Berkeley March.
Homology tutorial Hugh Hudson Solar MURI 21-Nov-03.
Page 1Hinode4 October 11-15, 2010 Studying Emerging Flux Regions With The SDO Data Yang Liu and HMI Team Stanford University and Other Places
The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.
Review of Conditions for the Formation and Maintenance of Filaments Paper by Sara F. Martin, 1998 Review presented by Samuel Tun October 13, 2005
1 Hinode Monthly Highlights – Slow Solar Wind Sources Derived from recent publication from the Hinode/EIS team through the Naval Research Laboratory EIS.
Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.
A topological view of 3D global magnetic field reversal in the solar corona Rhona Maclean Armagh Observatory 5 th December 2006.
The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.
Synoptic Solar Cycle observed by Solar Dynamics Observatory Elena Benevolenskaya Pulkovo Astronomical Observatory Saint Petersburg State University ‘Differential.
Proxies of the Entire Surface Distribution of the Photospheric Magnetic Field Xuepu Zhao NAOC, Oct. 18, 2011.
Intriguing Observations of a Failed Eruption? We present observations of a (partially) failed eruption of a magnetic flux rope following an M9.3 flare.
Probing Energy Release of Solar Flares M. Prijatelj Carnegie Mellon University Advisors: B. Chen, P. Jibben (SAO)
RHESSI and Radio Imaging Observations of Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD G. Trottet, Observatoire.
18-April-2006XRT Team1 Initial Science Observations Solar-B XRT Ed DeLuca for the XRT Team.
Coronal hard X-ray sources and associated decimetric/metric radio emissions N. Vilmer D. Koutroumpa (Observatoire de Paris- LESIA) S.R Kane G. Hurford.
Small scale magnetic energy release driven by supergranular flows Hugh Potts, Joe Khan and Declan Diver How to automatically detect and analyse supergranular.
SHINE SEP Campaign Events: Long-term development of solar corona in build-up to the SEP events of 21 April 2002 and 24 August 2002 A. J. Coyner, D. Alexander,
Using the evolution of dimming regions to probe the global magnetic field topology A new interpretation of the 12 th May 1997 event G. Attrill 1, M. Nakwaki.
Analysis Magnetic Reconnection in Solar Flares: the Importance of Spines and Separators Angela Des Jardins 1, Richard Canfield 1, Dana Longcope 1, Emily.
Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane.
5. Walen Test analysis The Walen Test results for Cluster 3 are as expected for a reconnection event. The test over the leading edge shows a positive correlation.
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.
NoRH Observations of RHESSI Microflares M.R. Kundu, Dept. of Astronomy, University of Maryland, College Park, MD E.J.Schmahl, Dept. of Astronomy, University.
High resolution images obtained with Solar Optical Telescope on Hinode
XRT and EIS Observations of Reconnection associated Phenomena D. Shiota, H. Isobe, D. H. Brooks, P. F. Chen, and K. Shibata
SHINE Formation and Eruption of Filament Flux Ropes A. A. van Ballegooijen 1 & D. H. Mackay 2 1 Smithsonian Astrophysical Observatory, Cambridge,
Coronal and Interplanetary Magnetic Fields in October-November 2003 and November CMEs Vasyl Yurchyshyn Big Bear Solar Observatory,
1 Yongliang Song & Mei Zhang (National Astronomical Observatory of China) The effect of non-radial magnetic field on measuring helicity transfer rate.
X Visit For 100’s of free powerpoints.
Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane.
What we can learn from active region flux emergence David Alexander Rice University Collaborators: Lirong Tian (Rice) Yuhong Fan (HAO)
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
Long-term measurements of the Sun’s poles show that reversal of the dominant magnetic polarity generally occurs within a year of solar maximum. Current.
Observations of Filament Channels by Hinode/XRT and STEREO
Studies on Twisted Magnetic Flux Bundles
GOAL: To understand the physics of active region decay, and the Quiet Sun network APPROACH: Use physics-based numerical models to simulate the dynamic.
Magnetic Topology of the 29 October 2003 X10 Flare
Exploring Large-scale Coronal Magnetic Field Over Extended Longitudes With EUVI EUVI B EIT EUVI A 23-Mar UT Nariaki Nitta, Marc DeRosa, Jean-Pierre.
XRT Particle Acceleration at Magnetic Reconnection Sites
Observations of emerging and submerging regions with ASP and Solar-B
Magnetic connection between the photosphere and the corona
Slit and Slot Interchange
Filament/Prominence Eruption Corona Mass Ejection (CME)
Fig. 2 Synoptic maps showing the varying properties of the corona and photosphere over a whole solar rotation. Synoptic maps showing the varying properties.
Presentation transcript:

Interaction between emerging flux and large scale loop systems observed with Hinode XRT Abstract Hinode XRT reveals ubiquitous large-scale connections between solar active regions and relatively distant reaches of the corona, both quiet and active. How do these large scale connections form? Data from the first several months of the mission suggest that large-scale connections tend to exist prior to active region emergence, rather than being due to long-term diffusion of a single active region. We describe the life-history of two large-scale loop systems. We find that they cyclically decay and reform due to repeated flux emergence in approximately the same location through successive solar rotations. We present a detailed look at the effect of flux emergence on the existing loop systems and the nature of the magnetic reconnection that takes place. Hinode takes full-disk synoptics every six hours in order to view large- scale phenomena. Long loops are ubiquitous in both quiet and active regions of Hinode observations. Here, an active region takes up > 30% of the visible disk.

Due to extremely broad temperature coverage and high spatial resolution, Hinode XRT is an exceptional instrument for studying large-scale solar magnetic connections and their interaction with smaller elements. The first and second panels at left show a pair of active regions with strong initial interconnection. Over the next five solar rotations, the region interconnectivity remains long after the regions themselves have dispersed. The large-scale structures are partly re-created due to repeated flux emergence in the same general location. Long-lasting Connections MDI Magnetogram After 3 rotationsAfter 4 rotationsAfter 5 rotations Initial Active RegionsAfter 2 rotations

Active Region Interactions A loop system that persists through one rotation (as well as substantial flaring from the active region in the west). New flux emerges into the middle of the resulting large loop scale structure after two solar rotations, which alters the remaining large-scale structure, though it remains relatively intact after 3 rotations. The loop system remains visible even in XRT's thin Be filter in panel (b), indicating a relatively high temperature component. After 2 rotationsAfter 3 rotations Initial Active RegionsAfter 1 rotation

Loraine L. Lundquist and the US & Japan XRT Teams Harvard/Smithsonian Center for Astrophysics Flux emerging into pre-existing loop connections, Part 1 Here we show a time series of emergence into the larger loop structure shown in the middle page on the left. The initial flux emergence interacts in a complex manner with the overlying arcade, but by the time the emergence matures, the overlying loops conform roughly to the same loop-structure of the newly formed active region. Thus the large spatial extent of the region is due not to loops extended from the emergence process, but from interaction with pre-existing connections.

A second time-series of emergence into an arcade. In this case, the flux emerges just into the footpoint of the arcade. The result is reconnection that results in shrinking the loops. Unlike the previous example this case results in an overall shortening of overlying loops rather than a broadening of the emerging region’s spatial extent. Flux emerging into pre-existing loop connections, Part 2 Time

MDI magnetogram contours (green = positive, blue = negative) are overlayed on the XRT data from the previous page. White dotted lines show the original arcade and the reconnection that occurs as a result of flux emergence. The same process occurs on two scales: first with the larger flux emergence of the whole region, and second with a tiny bipole of flux that emerges to the north of the primary active region. Reconnection Topology Time Summary Large scale loop systems last long after their counterpart active regions and are often visible even at relatively high temperatures. Repeated emergence may fuel these persistent structures. A likely cause for the large spatial extent of many active regions is reconnection with these pre-existing structures, rather than inherent size structure.