The detedction of photospheric impacts from chromospheric impulsive events Moretti,P.F. et al.,2003,ApJL,589,109 Short review 2003.09.08 神尾精.

Slides:

Advertisements

Similar presentations

L. Teriaca, IMPRS Seminar, Lindau 08/12/04 Spectroscopy of the solar Transition Region and Corona L. Teriaca.

Advertisements

S.L. Guglielmino eHeroes 3 rd General Meeting Davos – March, 2014 High resolution spectro-polarimetric observations of a delta spot hosting eruptive.

Analysis of a C4.1 flare occurred in a δ spot using SDO and SST data

August 22, 2006IAU Symposium 239 Observing Convection in Stellar Atmospheres John Landstreet London, Canada.

Nonlinearity of the force-free parameter over active regions. M.Hagino and T.Sakurai National Astronomical Observatory of Japan, Solar Observatory.

TRACE and RHESSI observations of the failed eruption of the magnetic flux rope Tomasz Mrozek Astronomical Institute University of Wrocław.

1 Plasma flows during solar flares A. Berlicki Observatoire de Paris, Section de Meudon, LESIA (Astronomical Institute of the Wrocław University, Poland)

A complete study of magnetic flux emergence, interaction, and diffusion should take into account some “anomalies” In the photosphere we can observe flux.

A complete study of magnetic flux emergence, interaction, and diffusion should take into account some “anomalies” In the photosphere we can observe flux.

Dark Energy in the Solar Corona H.S. Hudson, UCB & SPRC LMSAL, January 31, 2002.

Ryan Payne Advisor: Dana Longcope. Solar Flares General  Solar flares are violent releases of matter and energy within active regions on the Sun.  Flares.

SSPVE Discussion Group B Question 5 To what extent is it possible to predict the emergence of active regions before they reach the photosphere, or to predict.

Multiwavelength Study of Magnetic Reconnection Associated with Sigmoid Eruption Chang Liu BBSO/NJIT

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.

1Yang LiuCISM All-hand meeting CISM All-hand Meeting Yang Liu – Stanford University

1 Sunspot Studies in Oslo with CDS,SUMER,MDI and TRACE A final report (maybe). Per Maltby NilsBrynildsen Olav Kjeldseth-Moe, Per Maltby, Terje Fredvik.

DOPPLER DOPPLER A Space Weather Doppler Imager Mission Concept Exploration Science Objectives What are the most relevant observational signatures of flare,

Detection of Emerging Sunspot Regions in the Solar Interior Stathis Ilonidis, Junwei Zhao, and Alexander Kosovichev Stanford University LoHCo Workshop.

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.

Physics 681: Solar Physics and Instrumentation – Lecture 17 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

Multiheight Analysis of Asymmetric Stokes Profiles in a Solar Active Region Na Deng Post-Doctoral Researcher at California State University Northridge.

S.L. Guglielmino eHeroes Final Meeting Leuven – 8 th February 2015 Analysis of a C4.1 flare occurred in a δ spot S.L. Guglielmino 1, F. Zuccarello 1, P.

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.

A complete study of magnetic flux emergence, interaction, and diffusion should take into account some “anomalies” In the solar photosphere we can observe.

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,

By: Kiana and Meagan. Purpose  To measure solar magnetic fields  To understand how energy generated by magnetic-field changes in the lower solar atmosphere.

Quick changes of photospheric magnetic field during flare-associated surges Leping Li, Huadong Chen, Suli Ma, Yunchun Jiang National Astronomical Observatory/Yunnan.

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.

Locarno, 8 June 2005Peter Gallagher (UCD) Chromospheric Evaporation Peter Gallagher University College Dublin Ryan Milligan Queens University Belfast.

The Relation between Soft X-ray Ejections and Hard X-ray Emission on November 24 Flare H. Takasaki, T. Morimoto, A. Asai, J. Kiyohara, and K. Shibata Kwasan.

Probing Energy Release of Solar Flares M. Prijatelj Carnegie Mellon University Advisors: B. Chen, P. Jibben (SAO)

Micro-Flare and High-Speed Down-Flow observed with VTT R. Kano(1), Y. Katsukawa(1), Y. Kitakoshi(2), T. Shimizu(3), S. Tsuneta(1) and V. Martinez Pillet(4)

Chromospheric Magnetic Reconnection from an Observer’s Point of View Jongchul Chae Seoul National University, Korea.

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

Simultaneous optical and X-ray observations of flares and rotational modulation on the RS CVn binary HR 1099 (V711 Tau) from the MUSICOS 1998 campaign.

Measurement of the Reconnection Rate in Solar Flares H. Isobe 2004/12/6 Taiyo-Zasshikai.

Spectral Signature of Emergent Magnetic Flux D1 神尾精 Solar Seminar Balasubramaniam,K.S., 2001, ApJ, 557, 366. Chae, J. et al., 2000, ApJ, 528,

Multi-wavelength analysis of the impact polarization of 2001, June 15 th solar flare Zhi XU (1), Jean-Claude HENOUX (2), and Cheng FANG (3) (1) Yunnan.

Line Profile Characteristics of Solar Explosive Event Bursts Z. Ning et al 2004 A&A 419,1141 Speaker: Jinping Dun.

1. Twist propagation in Hα surges Patricia Jibben and Richard C. Canfield 2004, ApJ, 610, Observation of the Molecular Zeeman Effect in the G Band.

Local Helioseismology LPL/NSO Summer School June 11-15, 2007.

Solar seminor: 4 Oct (1)Eruption of a multiple-turn helical magnetic flux tube in a large flare : Evidence for external and i ternal reconnection.

High resolution images obtained with Solar Optical Telescope on Hinode

Ganghua Lin Huairou Solar Observating Station,NAO,CAS.

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

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)

Fabry-Perot Approach to SPRING Sanjay Gosain NSO.

The HMI Instrument. HMI Science Goals Line-of-Sight Observables.

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

Focal Plane Instrumentation at Big Bear Solar Observatory

Dong Li Purple Mountain Observatory, CAS

Marina Battaglia, FHNW Säm Krucker, FHNW/UC Berkeley

Planning Flare Observations for Hinode/EIS

Diagnostic of Chromospheric Flare Plasma

Dynamics of the lower solar chromosphere using CRISP-SST data Arnold Hanslmeier(1), Teimuraz Zaqarashvili (1), Julius Koza (2), Jan Rybak (2) (1) Institut.

TRACE Downflows and Energy Release

Motions of isolated G-band bright points in the solar photosphere

Downflows and Plasmoid Ejections as a Reconnection Outflow

Evolution of Ha Flare Kernels and Energy Release

Teriaca, et al (2003) ApJ, 588, SOHO/CDS HIDA/DST 2002 campaign

Chromospheric and Transition Region Dynamics

High-cadence Radio Observations of an EIT Wave

Understanding solar flares from optical observations Heinzel, P

Calibration and Analysis of Ha Data to be Taken by SOT/NFI

This waveform is 35.0 cm long. How long is the wavelength?

Solar magnetic elements at 0

Poster L2 Filtergraph calibration for the Polarimetric and Helioseismic Imager Solar Orbiter Carlos DOMINGUEZ-TAGLE, et al Institut d’Astrophysique Spatiale,

Slit and Slot Interchange

Presentation transcript:

The detedction of photospheric impacts from chromospheric impulsive events Moretti,P.F. et al.,2003,ApJL,589,109 Short review 2003.09.08 神尾精

Abstract Perturbation of photosphere caused by chromospheric impulsive downflow is detected. Although it is generally accepted that convective flow is the source of solar oscillation, the downflow events may be the origin of solar oscillation.

Instrument Italian Panoramic Monochrometer (IPM) installed in THEMIS. Birefringent ＋ Fabry Perot Filters Cd isotope for wavelength reference  Precision of about 10 m/s (～2mÅ) Wavelength range 4600Å～6800Å

Observation B class flare in AR 9455 at 10:00UT on 2001 May 13 Images of 11 wavelengths were obtained each 40s. Fe I 5576.1Å 0, ±45, ±80 mÅ Na I 5889.97Å 0, ±80 mÅ Hα 6562.8Å 0, ±650 mÅ Dopplergrams were obtained by fitting FeI images with Gaussian profile

Hα and acceleration map Trigger Area(TRA) First Brightening Area(FBA) Hα line core image Acceleration map of FeI Strong acceleration is detected in FBA and TRA

Time plot Flare started at 09:58 UT Impulsive down flow at 10:10 UT wing core

Velocity and FWHM of FeI 09:40 FWHM increase 09:52 Upflow in TRA 09:58 Flare start in FBA(Hα) 10:10 Downward pulse

Discussion Downward flows in the photosphere are detected during a B-class flare. Upward flow seems to be related to the trigger of the flare. Kinetic energy released by the downflow jet is approximately 5x1026 erg. These events are the part of the source of solar oscillation.