Science With the Extreme-ultraviolet Spectrometer (EIS) on Solar-B by G. A. Doschek (with contributions from Harry Warren) presented at the STEREO/Solar-B.

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

000509EISPDR_SciInvGIs.1 EIS Performance and Operations Louise Harra Mullard Space Science Laboratory University College London.
Masuda Flare: Remaining Problems on the Looptop Impulsive Hard X-ray Source in Solar Flares Satoshi Masuda (STEL, Nagoya Univ.)
Physical characteristics of selected X-ray events observed with SphinX spectrophotometer B. Sylwester, J. Sylwester, M. Siarkowski Space Research Centre,
Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team.
1 Hinode Coordinated Observations: Heat Transfer Contributed by the Hinode/EIS team through the Naval Research Laboratory and University College London.
Energy Release and Particle Acceleration in Flares Siming Liu University of Glasgow 9 th RHESSI Workshop, Genova, Italy, Sep
1 Plasma flows during solar flares A. Berlicki Observatoire de Paris, Section de Meudon, LESIA (Astronomical Institute of the Wrocław University, Poland)
Multi-Wavelength Studies of Flare Activities with Solar-B ASAI Ayumi Kwasan Observatory, Kyoto University Solar-B Science February 4, 2003.
The Sun’s Dynamic Atmosphere Lecture 15. Guiding Questions 1.What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere.
000509EISPDR_SciInvGIs.1 EIS Science Goals: The First Three Months…. Louise Harra Mullard Space Science Laboratory University College London.
Estimating the Chromospheric Absorption of Transition Region Moss Emission Bart De Pontieu, Viggo H. Hansteen, Scott W. McIntosh, Spiros Patsourakos.
SH13A-2240 Automatic Detection of EUV Coronal Loops from SDO-AIA Data Alissa N. Oppenheimer¹ ( ), A. Winebarger², S. Farid³,
MSU Solar Physics REU Jennifer O’Hara Heating of Flare Loops With Observationally Constrained Heating Functions Advisors Jiong Qiu, Wenjuan Liu.
XRT X-ray Observations of Solar Magnetic Reconnection Sites
White-Light Flares: TRACE and RHESSI Observations H. Hudson (UCB), J. Wolfson (LMSAL) & T. Metcalf (CORA)
Measuring the Temperature of Hot Solar Flare Plasma with RHESSI Amir Caspi 1,2, Sam Krucker 2, Robert P. Lin 1,2 1 Department of Physics, University of.
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.
Properties of Prominence Motions Observed in the UV T. A. Kucera (NASA/GSFC) E. Landi (Artep Inc, NRL)
SDO/AIA science plan: prioritization and implementation: Five Objectives in 10 steps [session no.] HMI/AIA science teams meeting; Monterey; Feb
Flares and Eruptive Events Observed with the XRT on Hinode Kathy Reeves Harvard-Smithsonian Center for Astrophysics.
Solar-B Science Objectives - Overview of the Mission - Kazunari Shibata (Kyoto Univ.)
990901EIS_RR_Science.1 Science Investigation Goals and Instrument Requirements Dr. George A. Doschek EIS US Principal Investigator Naval Research Laboratory.
Solar-B/EIS high-cadence observation for diagnostics of the corona and TR S. Kamio (Kyoto Univ.) Solar-B domestic meeting.
1 Future solar missions (Based on the summary by R.A. Harrison) S. Kamio
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.
EIS - MSSL/NRL EUV Imaging Spectrometer SOT - ISAS/NAOJ Solar Optical Telescope XRT - SAO/ISAS X-ray Telescope FPP - Lockheed/NAOJ Focal Plane Package.
Evolution of Flare Ribbons and Energy Release Rate Ayumi Asai 1,2, T. Yokoyama T. 3, M. Shimojo 2, S. Masuda 4, and K. Shibata 1 1:Kwasan and Hida Observatories,
High Resolution Imaging and EUV spectroscopy for RHESSI Microflares S. Berkebile-Stoiser 1, P. Gömöry 1,2, J. Rybák 2, A.M. Veronig 1, M. Temmer 1, P.
Magnetic Reconnection in Flares Yokoyama, T. (NAOJ) Reconnection mini-workshop Kwasan obs. Main Title 1.Introduction : Reconnection Model of.
18-April-2006XRT Team1 Initial Science Observations Solar-B XRT Ed DeLuca for the XRT Team.
Where is Coronal Plasma Heated? James A. Klimchuk NASA Goddard Space Flight Center, USA Stephen J. Bradshaw Rice University, USA Spiros Patsourakos University.
TESIS on CORONAS-PHOTON S. V. Kuzin (XRAS) and TESIS Team.
Observations of Moreton waves with Solar-B NARUKAGE Noriyuki Department of Astronomy, Kyoto Univ / Kwasan and Hida Observatories M2 The 4 th Solar-B Science.
Studies on the 2002 July 23 Flare with RHESSI Ayumi ASAI Solar Seminar, 2003 June 2.
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.
Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane.
Evolution of Flare Ribbons and Energy Release Rate Ayumi ASAI 1, Takaaki YOKOYAMA 2, Masumi SHIMOJO 3, Satoshi MASUDA 4, and Kazunari SHIBATA 1 1:Kwasan.
Spectroscopic Detection of Reconnection Evidence with Solar-B II. Signature of Flows in MHD simulation Hiroaki ISOBE P.F. Chen *, D. H. Brooks, D. Shiota,
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.
Emission measure distribution in loops impulsively heated at the footpoints Paola Testa, Giovanni Peres, Fabio Reale Universita’ di Palermo Solar Coronal.
Coronal loops: new insights from EIS observations G. Del Zanna 1,2, S. Bradshaw 3, 1 MSSL, University College London, UK 2 DAMTP, University of Cambridge,
Determining the Heating Rate in Reconnection Formed Flare Loops Wenjuan Liu 1, Jiong Qiu 1, Dana W. Longcope 1, Amir Caspi 2, Courtney Peck 2, Jennifer.
Flare Prediction and the Background Corona Coronal Diagnostic Spectrometer Wolter-Schwarzschild Type 2 telescope Two separate spectrometers- the Normal.
Probing Electron Acceleration with X-ray Lightcurves Siming Liu University of Glasgow 9 th RHESSI Workshop, Genova, Italy, Sep
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
Model instruments baseline specification and key open issues EUV/FUV High-Throughput Spectroscopic Telescope Toshifumi Shimizu (ISAS/JAXA) SCSDM-4.
Flare Irradiance Studies with the EUV Variability Experiment on SDO R. A. Hock, F. G. Eparvier, T. N. Woods, A. R. Jones, University of Colorado at Boulder.
XUV monochromatic imaging spectroscopy in the SPIRIT experiment on the CORONAS-F mission I. Diagnostics of solar corona plasma by means of EUV Spectroheliograph.
2005/11/15STEREO/Solar-B Workshop1 Solar-B X-ray Telescope (XRT) R. Kano (NAOJ) and XRT Team XRT.
Flare Ribbon Expansion and Energy Release Ayumi ASAI Kwasan and Hida Observatories, Kyoto University Explosive Phenomena in Magnetized Plasma – New Development.
RHESSI and the Solar Flare X-ray Spectrum Ken Phillips Presentation at Wroclaw Workshop “ X-ray spectroscopy and plasma diagnostics from the RESIK, RHESSI.
Nov. 8-11, th Solar-B science meeting Observational Analysis of the Relation between Coronal Loop Heating and Photospheric Magnetic Fields Y. Katsukawa.
Flares and Eruptive Events Observed with the XRT on Hinode Kathy Reeves Harvard-Smithsonian Center for Astrophysics.
Observations of the Thermal and Dynamic Evolution of a Solar Microflare J. W. Brosius (Catholic U. at NASA’s GSFC) G. D. Holman (NASA/GSFC)
On the spectroscopic detection of magnetic reconnection evidence with Solar B – I. Emission line selection and atomic physics issues P. F. Chen 1,2, H.
Active Region Loops - Observational Constraints on Heating from Hinode/EIS Observations Helen E. Mason DAMTP, Centre for Mathematical Sciences, University.
2 nd Solaire Network Meeting Catania, January 2009 Investigating the characteristics of coronal loop heating by 1D hydrodynamic simulations R.
Evolution of Flare Ribbons and Energy Release Ayumi ASAI 1, Takaaki YOKOYAMA 2, Masumi SHIMOJO 3, Satoshi MASUDA 4, Hiroki KUROKAWA 1, and Kazunari SHIBATA.
Spectroscopic Observations with SolarB-EIS Helen E. Mason DAMTP, Centre for Mathematical Sciences Giulio Del Zanna, MSSL.
November 18, 2008Jonathan Cirtain SCIENCE & MISSION SYSTEMS Solar-C Plan ‘A’ Coronal observations Jonathan Cirtain MSFC/NASA November 18, 2008.
Studies on Twisted Magnetic Flux Bundles
Planning Flare Observations for Hinode/EIS
Emission measure distribution from plasma modeling
Evolution of Flare Ribbons and Energy Release
Motions of isolated G-band bright points in the solar photosphere
Teriaca, et al (2003) ApJ, 588, SOHO/CDS HIDA/DST 2002 campaign
Understanding solar flares from optical observations Heinzel, P
Downflow as a Reconnection Outflow
Presentation transcript:

Science With the Extreme-ultraviolet Spectrometer (EIS) on Solar-B by G. A. Doschek (with contributions from Harry Warren) presented at the STEREO/Solar-B Science Planning Workshop November 2005 Turtle Bay, Oahu, Hawaii

Solar-B Extreme-Ultraviolet Imaging Spectrometer (EIS) EIS reveals the dynamics, temperature, density, and composition of the emitting plasma, information crucial for understanding the physics of the solar atmosphere. Spectra are obtained with high spatial resolution (~ 730 km), i.e., spectra at many locations within an entire solar structure can be recorded. Spectra are obtained with sufficient time resolution (seconds) to determine physical parameters as a function of position within magnetic loops without significant ambiguity due to temporal changes within the structures. Spectra can be accurately related to images obtained from the Solar-B White Light and X-Ray Telescopes, for context purposes. EIS is the first EUV solar spectrometer capable of obtaining high spectral resolution data with both high spatial and temporal resolution.

EIS Spatial resolution = 2”, 1” pixels Spectral resolution = Å/pixel SERTS Spatial resolution = 5” Spectral resolution = Å in first order, Å in second order Skylab Spatial resolution = 2-3” Spectral resolution = Å/2” spatial resolution element EIS Spatial and Spectral resolution

EIS: The Use of Slits and Slots Skylab flare spectral images and EIS 40” wide slot Solar M3 flare time sequence Slit spectra give line profiles

Example of EIS Science: Solar Flares Test the magnetic reconnection model of solar flares Understand the structure of multi-million degree flare loops. Why are there confined bright regions at the tops of loops? Specifically, what is the extent of their boundary regions? Resolve the apparent discrepancies between numerical simulations of flare loops and observations of multimillion degree upflows due to chromospheric evaporation.

The Elusive Reconnection Region Observe motions of ejecta and inflows above arcade –Requires cooler lines and longer exposures – summing of images From Sheeley, Warren, and Wang, ApJ, 2004 From Shibata et al., ApJ, 1995

Images of Multi-million Degree Flare Loops Do flare loops at temperatures of MK look like what we expect??? –No, they don’t, but as they cool to 1-3 MK they look more and more like respectable 1D loops should. TRACE observations confirm the gross flare loop morphology seen by Yohkoh; EIS will enable the detailed temperature structure of flare loops to be determined.

Solar Flare Reconnection Model This schematic flare model provides theoretical guidance for analyzing solar flare data. Solar flare 45,000 km

FLARE STRUCTURE EIS will enable the flare structure and distribution of physical parameters such as temperature in flare loops to be measured. Skylab imaging spectra Spectral line intensity ratios of Fe XXIII/Fe XXIV (263/255) and Fe XXII/Fe XXIV (247/255) will allow the spatial extent of the bright knot boundaries to be determined.

Chromospheric Evaporation: Ca XIX X-ray Spectra

A Multi-Thread Flare Loop Model The overall soft X-ray magnetic flare envelop is assumed to be composed of sub-resolution magnetic “threads”. Idea due to Hori, Takaaki, Kosugi, & Shibata (ApJ, 500, 492 (1998)). The threads are modeled as individual flare loops using the NRL 1D solar flux tube model. The flare onset is modeled as a succession of independently heated threads. The length of the flare loop is determined by observations of the overall magnetic envelop. The energy deposited in each thread and its cross-sectional area are related to the GOES fluxes (Warren & Antiochos 1994). The energy in each successively heated thread is determined such that the X-ray flux matches the GOES light curves. The BCS spectrometers on Yohkoh serve as a completely independent test of the model. The BCS data support the multi-thread model (Warren & Doschek 2005, ApJ, 618, L157).

A Multi-Thread Flare Loop Simulation Observe evolution and distribution of multi- temperature plasma –Requires images that span 10 4 – 10 7 K. From Warren & Doschek, ApJ, 2005

One Flare Observing Procedure Use 250” slot, center EIS slot on magnetic neutral line of a magnetically complex active region. Use EIS or XRT flare trigger to signify onset of a flare. Select eight wavelength windows of 2.5’x2.5’ in size, in spectral lines of Fe XXIV (192, 255), Fe XXIII (263), FeXXII (247), Ca XVII (192), Fe XV (284), Fe XII (195), and He II (256). Readout windows in 10s time intervals for 0.5 hours after flare onset. Obtain good data sets for both disk and limb events.

Data Reduction and Analysis Program Co-register monochromatic flare images to within 1” –Optical properties of EIS –Context images (e.g., Fe XII), and XRT images –Auto-correlation techniques Determine structure of flare and physical parameters (e.g., temperature) from the data –EIS point spread function, filling factors Comparison of results with theoretical numerical simulations –NRL 1D Dynamic Flux Tube Model, NRL ARMS Code –Modifications to numerical simulation codes

Questions How do we optimize exposure time? –Avoid saturation of bright lines –This may lead to underexposure of weak lines –Improve signal-to-noise by summing? How do we optimize cadence? –We want many windows and high cadence –Telemetry is limited –Image compression?