2009/06/22XRT Team Meeting1 A Proposal of Standard Observations: AR, Flare, and PreFlare R. Kano (NAOJ)

Slides:

Advertisements

Similar presentations

Sec 1-4 Concepts: Classifying Angles Objectives: Given an angle, name, measure and classify it as measured by a s.g.

Advertisements

EIS/Solar-B: 3. Electrical Interface to MDP EISMDP PIM HK PIM DHU DR analog data (temperature, current, etc.) S/C bus image compression status data command.

000509EISPDR_SciInvGIs.1 EIS Performance and Operations Louise Harra Mullard Space Science Laboratory University College London.

XRT Instrument Capabilities Ed DeLuca, Leon Golub & Jay Bookbinder SAO.

Physical characteristics of selected X-ray events observed with SphinX spectrophotometer B. Sylwester, J. Sylwester, M. Siarkowski Space Research Centre,

Probing Magnetic Reconnection with Active Region Transient Brightenings Martin Donachie Advisors: Adam Kobelski & Roger Scott.

Instrument Checkout / Performance Verification for XRT & Control of XRT Observation R. Kano for the XRT Team.

2007/12/08-10Hinode Workshop in China1 HINODE/X-Ray Telescope R. Kano （ NAOJ ） & Japan-US XRT Team Golub et al. “The X-Ray Telescope (XRT) for the Hinode.

2007/12/08-10Hinode Workshop in China 1 XRT Analysis Software R. Kano (NAOJ) and XRT Teams.

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.

XRT-MDP Functions - AEC · ARS · FLD - Masumi Shimojo Nobeyama Solar Radio Observatory 4th Solar-B Science Meeting

2007/12/08-10 Hinode Workshop / Hinode 専題研討会 1 XRT Observation Planning R.Kano (NAOJ) and XRT team.

6/2/2015 Solar-B XRT XRT-1 A High Resolution Grazing Incidence Telescope for the Solar-B Observatory Solar-B XRT Presenter: Leon Golub Smithsonian Astrophysical.

XRT X-ray Observations of Solar Magnetic Reconnection Sites

Soft X-ray observations of global waves Khan-Aurass 2002 Narukage et al Hudson et al

Vincent Surges Advisors: Yingna Su Aad van Ballegooijen Observations and Magnetic Field Modeling of a flare/CME event on 2010 April 8.

The Change of Magnetic Inclination Angles Associated with Flares Yixuan Li April 1,2008.

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.

Direct Evidence of Emergence of a Helical Flux Rope under an Active- Region Prominence Joten Okamoto Kyoto Univ. ／ NAOJ JSPS Research Fellow Saku Tsuneta,

Preflare physical conditions inferred from Hinode Hugh Hudson (UC Berkeley) and Ed DeLuca (CfA)

990901EIS_RR_Science.1 Science Investigation Goals and Instrument Requirements Dr. George A. Doschek EIS US Principal Investigator Naval Research Laboratory.

METHOD OF DEM ESTIMATION 1.Generating “true” model observations. We start with the XRT temperature response functions R c (T) and a coronal emission model.

New Views of the Solar Corona with Hinode X-Ray Telescope (XRT) Taro Sakao (ISAS/JAXA) and the XRT Team (ISAS/JAXA, SAO, NAOJ, NASA/MSFC)

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.

Solar observation modes: Commissioning and operational C. Vocks and G. Mann 1. Spectrometer and imaging modes 2. Commissioning proposals 3. Operational.

“Joint planning” session Preliminary instrument operation & science plans of SOT/XRT/EIS for several months after the launch. Instrument checkout and Performance.

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.

2005/11/086th Solar-B Science Supersonic downflows in the photosphere discovered in sunspot moat regions T. Shimizu (ISAS/JAXA, Japan),

TESIS on CORONAS-PHOTON S. V. Kuzin (XRAS) and TESIS Team.

Space and Astrophysics Solar B as a tool for coronal wave studies Solar B as a tool for coronal wave studies Valery M. Nakariakov University of Warwick.

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.

XRT’s Observational Parameters R. Kano (NAOJ). Contents FOV & Full Disk Imaging Time Cadence & Observation Table New Items as Solar X-ray Telescopes –Pre-flare.

Subaru/FMOS Commissioning: Brief history & current status Naoyuki Tamura Instrument scientist Subaru Telescope, NAOJ Expected performance Observation “A.

NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.

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.

Flare-associated shock waves observed in soft X-ray NARUKAGE Noriyuki Kwasan and Hida Observatories, Kyoto University – DC3 The 6 th Solar-B Science Meeting.

Comments for a preliminary EIS science plan H. Hara 2005 Oct 31 For the science meeting at ISAS.

Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane.

SNAP Collaboration meeting / Paris 10/20071 SPECTROMETER DETECTORS From science requirements to data storage.

XRT vs. AIA Synoptics Yingna Su 2011-Jan-25. We take a look at the recent XRT 9-filter synoptic observations on Jan 5 (12 UT), Jan 9 (20 UT), and Jan.

台灣清華大學，物理系 Helioseismology (II) Global and Local Helioseismology ( , 北京 ) 周定一 Dean-Yi Chou.

KASI Low atmospheric reconnections associated with an eruptive flare Yong-Jae Moon(1), Jongchul Chae(2), Young-Deuk Park(1) 1: Korea Astronomy and.

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,

Acoustic wave propagation in the solar subphotosphere S. Shelyag, R. Erdélyi, M.J. Thompson Solar Physics and upper Atmosphere Research Group, Department.

Examples of SOT Observation in Performance Verification Phase M. Kubo (JAXA/ISAS) and SOT team.

The Behavior of Waves. Reflection Reflection – when a wave strikes an object and bounces off of it All types of waves can be reflected.

IMAGING AND SPECTOROPIC INVESTIGATIONS OF A SOLAR CORONAL WAVE: PROPERTIES OF THE WAVE FRONT AND ASSOCIATED ERUPTING MATERIAL L OUISE K. HARRA AND A LPHONSE.

2005/11/15STEREO/Solar-B Workshop1 Solar-B X-ray Telescope (XRT) R. Kano (NAOJ) and XRT Team XRT.

Takashi Sekii NAOJ SOT observing modes for local helioseismology and data analysis.

Flares and Eruptive Events Observed with the XRT on Hinode Kathy Reeves Harvard-Smithsonian Center for Astrophysics.

The X-Ray Telescope aboard Solar-B: An Overview Taro Sakao (ISAS/JAXA) and The XRT Team.

Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane.

Differential Rotation of coronal BP and Source Region of their Magnetic Fields H. Hara NAOJ 2011 Jun 29 Leverhulme – Probe the Sun 1 st Workshop at MSSL.

Discussion Points for CME Group A. Vourlidas NRL.

Investigating a complex X-class flare using NLFFF modeling

P.Zacharias1, S. Bingert2 & H. Peter2 1ISSI, Bern, Switzerland

Planning Flare Observations for Hinode/EIS

Lunar observation data set preparation

VIRTIS Operations at Lutetia

Roy Coulter Institute for Astronomy/ UH

High-cadence Radio Observations of an EIT Wave

Flare-Associated Oscillations Observed with NoRH

Flare Ribbon Expansion and Energy Release

MDP / DHU - DR Usage vs downlinks -

Downflow as a Reconnection Outflow

Structure and Dynamics in Sunspot Light Bridges

Basics of fMRI and fMRI experiment design

Periodic Acceleration of Electrons in Solar Flares

Presentation transcript:

2009/06/22XRT Team Meeting1 A Proposal of Standard Observations: AR, Flare, and PreFlare R. Kano (NAOJ)

2009/06/22XRT Team Meeting2 Concept of Standard Obs. Active Region (AR) –Take 2(or 3)-filter images with 3 different FOVs (Core, Border and Environment) all day. It is because events in active regions often affect (or are affected by) their environments. This plan does not cover detail studies for multi-thermal (or DEM) structures. Special observations or collaborations with EIS will be needed for them. –Take AR Core with the ~1 min cadence. Because sound waves (~240km/s) take 5 min to travel along a loop (~100” = 73Mm), we can catch 5 phases of motions with sound speed in a loop. AR with PreFlare observation –The same observation, but with a rapid cadence for Core- and Border-FOVs by using preflare buffers. Flare (FL) –The same set of FOVs, but with a rapid cadence and thicker filters.

2009/06/22XRT Team Meeting3 A Baseline Plan for Standard AR Observation Core -FOV: 384”x384” -Res.: 1”x1” -Filter: G2 & G3 -Exp.: AEC3 (no sat.) -Cadence: 1 set / 1 min Border -FOV: 768”x768” -Res.: 2”x2” -Filter: G1, G2 & G3 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min Environment -FOV: 1024”x1024” -Res.: 4”x4” -Filter: G1 & G2 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min (Images were taken in a dry run in May. ) The 1 st dry run on May 23 revealed that we should reduce the data rate for continuous observations.

2009/06/22XRT Team Meeting4 Composite Image of 3 FOVs taken with Ti/poly. in the test on May 23 (see Appendix-1) 384”x384” 1024”x1024”

2009/06/22XRT Team Meeting5 Filter Groups G1 Al/mesh G2 Ti/poly. C/poly. Al/poly. G3 thin Be G4 med Al med Be G5 thick Al thick Be We classified the X-ray filters into 5 groups in this PPT, to simplify the proposal. thinnerthicker AR Core AR Border AR Env. FL Core FL Border FL Env.

2009/06/22XRT Team Meeting6 What is different from AR Obs? Core -FOV: 384”x384”=ROI-15 -Res.: 1”x1” -Filter: G2 & G3 -Exp.: AEC3 (no sat.) -Cadence: 1 set / 1 min Border -FOV: 768”x768”=ROI-16 -Res.: 2”x2” -Filter: G1, G2 & G3 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min Environment -FOV: 1024”x1024” -Res.: 4”x4” -Filter: G1 & G2 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min 30sec 1 min G4 & G5G2, G3 & G4 Flare Observation AR with PreFlare Observation Core -FOV: 384”x384” -Res.: 1”x1” -Filter: G2 & G3 -Exp.: AEC3 (no sat.) -Cadence: 1 set / 1 min Border -FOV: 768”x768”=ROI-5 -Res.: 2”x2” -Filter: G1, G2 & G3 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min Environment -FOV: 1024”x1024” -Res.: 4”x4” -Filter: G1 & G2 -Exp.: AEC2 (small sat.) -Cadence: 1 set / 2 min 30sec 1 min

2009/06/22XRT Team Meeting7 Schematic View of Time Cadences Core Border Env. Core Border Env. From AR obs. to FL obs. From AR+PreFlare obs. to FL obs. Stored in Preflare Buffers Overwritten in Preflare Buffers ~ 1 min~ 30 sec FL modeQT mode FL modeQT mode time Different colors mean different filters.

2009/06/22XRT Team Meeting8 Estimated Data Rate Based on the dry-run test using JPEG Q95 (see Appendix-2), the data rate of the baseline AR obs. is estimated to 3,057 Mbits/day. It is much larger than the recent DR volume allocated to XRT (800~900 Mbits/day). We would like to keep the concept. But, some modifications are necessary. For examples: –Reduce the cadence from 1min to 2min for Core, and from 2 min to 12min for Border & Env.  867Mbits/day –Reduce the FOV size to 256”x256” but keep the 1min cadence for Core. Reduce the cadence to 10min for Border & Env.  873Mbits/day –Reduce the JPEG-Q from 95 to 85 for Core and to 92 for Border & Env. For Border & Env., reduce the cadence to 5min also (see Appendix-3).  875Mbits/day

2009/06/22XRT Team Meeting9 Test Programs for AR(#16B4) & FL(#16B5) AR Core AR Border AR Env. G-band & Darks FL Core FL Border FL Env. G-band Appendix-1:

2009/06/22XRT Team Meeting10 Compression Rate median values derived in the test AR observation on May 23. Appendix-2: G3: thin BeG2: Ti/poly.G1: Al/mesh Core 384”x384”, 1”-Res. 19.5% 2.34bit/pix 24.6% 2.95bit/pix Border 768”x768”, 2”-Res. 21.1% 2.53bit/pix 42.2% 5.06bit/pix 54.9% 6.59bit/pix Env. 1024”x1024”, 4”-Res % 6.19bit/pix 50.0% 6.00bit/pix JPEG(Q=95) was used for all X-ray images. The data rate of the baseline AR obs. was estimated based on this compression rate and the parameters on slide 4.

2009/06/22XRT Team Meeting11 Smaller Q-values were tested on June 13. XOB#16B4thin BeTi/poly.Al/mesh Core16.4%20.7%----- Border23.5%44.8%54.5% Env %55.7% XOB#16C5thin BeTi/poly.Al/mesh Core 8.2%11.2%----- Border17.2%37.8%46.8% Env %48.0% Core: Q85 Env.: Q92 Border: Q92 Core: Q95 Env.: Q95 Border: Q95 Appendix-3: It looks okey.