Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory.

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

An overview of the cycle variations in the solar corona Louise Harra UCL Department of Space and Climate Physics Mullard Space Science.

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.

Nanoflares and MHD turbulence in Coronal Loop: a Hybrid Shell Model Giuseppina Nigro, F.Malara, V.Carbone, P.Veltri Dipartimento di Fisica Università della.

Free Magnetic Energy and Flare Productivity of Active Regions Jing et al. ApJ, 2010, April 20 v713 issue, in press.

Do active Regions Emerge in a Similar Regime? Valentyna Abramenko Valentyna Abramenko Big Bear Solar Observatory Big Bear Solar Observatory California,

Connections Between the Magnetic Carpet and the Unbalanced Corona: New Monte Carlo Models Steven R. Cranmer & Adriaan van Ballegooijen Harvard-Smithsonian.

Valentina Abramenko Big Bear Solar Observatory of NJIT Multi-fractality of Solar Magnetic Fields: New Progress with HMI Abstract. The SDO/HMI instrument.

MSU Team: R. C. Canfield, D. W. Longcope, P. C. H. Martens, S. Régnier Evolution on the photosphere: magnetic and velocity fields 3D coronal magnetic fields.

Intermittency in the Photosphere and Corona as Derived from Hinode Data Valentina Abramenko Vasyl Yurchyshyn Big Bear Solar Observatory of NJIT Haimin.

Rapid Changes in the Longitudinal Magnetic Field Associated with the July gamma -ray Flare Vasyl Yurchyshyn, Haimin Wang, Valentyna Abramenko,

Understanding Magnetic Eruptions on the Sun and their Interplanetary Consequences A Solar and Heliospheric Research grant funded by the DoD MURI program.

Statistical Distributions of Speeds of Coronal Mass Ejections 1 Big Bear Solar Obs, Big Bear, CA 92314; 2 Catholic University of America, Washington DC.

Multi-fractality of Solar Magnetic Fields: New Progress with HMI Valentina I. Abramenko Big Bear Solar Observatory of NJIT Poster #40.

Spatially Dependent Emergence Rate V. Abramenko. Outlook Compare results from the paper by Abramenko, Fisk, Yurchyshyn ApJ 641 (hereafter AFY) with that.

The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.

Changes of Magnetic Structure in 3-D Associated with Major Flares X3.4 flare of 2006 December 13 (J. Jing, T. Wiegelmann, Y. Suematsu M.Kubo, and H. Wang,

Distribution of the magnetic flux in elements of the magnetic field in an active region Valentyna Abramenko Big Bear Solar Observatory, NJIT.

Solar Wind Model at LMSAL AIA/HMI Science Team Meeting Session S3 15 February 2006 Marc DeRosa.

Study of magnetic helicity in solar active regions: For a better understanding of solar flares Sung-Hong Park Center for Solar-Terrestrial Research New.

Space Weather Forecast With HMI Magnetograms: Proposed data products Yang Liu, J. T. Hoeksema, and HMI Team.

V.I. Abramenko, V.B. Yurchyshyn, H. Wang, T.R. Spirock, P.R. Goode Big Bear Solar Observatory, NJIT Crimean Astrophysical Observatory, Ukraine

Calculation of Intermittency in the Photosphere and Corona from Hinode Data Valentina I. Abramenko And Vasyl B. Yurchyshyn Big Bear Solar Observatory of.

Photospheric Sources of Very Fast (>1100km/s) Coronal Mass Ejections Recent studies show that only very fast CMEs (> 1100 km/s) are capable of producing.

Magnetic Field and Heating of the Corona Valentyna Abramenko and Vasyl Yurchyshyn Big Bear Solar Observatory.

Coronal holes as seen in soft X-rays H. S. Hudson (UCB and SPRC) SOHO-11, Davos, March 13, 2002.

UCB MURI Team Introduction An overview of ongoing work to understand a well observed, eruptive active region, along with closely related studies…..

Pre-Flare Changes in Current Helicity and Turbulent Regime of the Photospheric Magnetic Field V.I. Abramenko Big Bear Solar Observatory,NJIT Crimean Astrophysical.

The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.

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

Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn Big Bear solar Observatory of NJIT, CA 2 – CSPAR, Univ. of Alabama in Nuntsville,

Thomas Zurbuchen University of Michigan The Structure and Sources of the Solar Wind during the Solar Cycle.

What coronal parameters determine solar wind speed? M. Kojima, M. Tokumaru, K. Fujiki, H. Itoh and T. Murakami Solar-Terrestrial Environment Laboratory,

The Asymmetric Polar Field Reversal – Long-Term Observations from WSO J. Todd Hoeksema, Solar Observatories H.E.P.L., Stanford University SH13C-2278.

Analysis of Coronal Heating in Active Region Loops from Spatially Resolved TR emission Andrzej Fludra STFC Rutherford Appleton Laboratory 1.

Observing the Sun. Corona: EUV; X-rays Chromosphere: H , UV, EUV Photosphere: near UV, Visible light, infra-red.

Observational Criteria for Small-Scale Turbulent Dynamo in the Solar Photosphere Valentina Abramenko, Philip Goode, Vasyl Yurchyshyn, Kwangsu Ahn Big Bear.

Semi-Empirical MHD Modeling of the Solar Wind Igor V. Sokolov, Ofer Cohen, Tamas I. Gombosi CSEM, University of Michigan Ilia I Roussev, Institute for.

1Yang Liu/Magnetic FieldHMI Science – 1 May 2003 Magnetic Field Goals – magnetic field & eruptive events Yang Liu Stanford University.

Signatures of Intermittent Turbulence in Hinode Quiet Sun Photosphere Valentina Abramenko, Big Bear Solar Observatory, USA, Plasma.

SLIDE SHOW 3 B changes due to transport + diffusion III -- * * magnetic Reynold number INDUCTION EQUATION B moves with plasma / diffuses through it.

Flare Energy Build-Up in a Decaying Active Region Near a Coronal Hole Yingna Su Smithsonian Astrophysical Observatory Collaborators: A. A. van Ballegooijen,

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

SOLAR FLARES AND ERUPTIONS Lyndsay Fletcher University of Glasgow.

The Sun The Sun imaged in white light by the SOHO spacecraft.

1 Abramenko V.I., 1 Yurchyshyn, V., 2 Linker, J., 2 Mikic, Z. 1 - Big Bear Solar Observatory of NJIT; 2 – Predictive Science Inc., San Diego Anomalous.

Flux Emergence Rate in Coronal Holes and in Adjacent Quiet-sun Regions Valentyna Abramenko Big Bear Solar Observatory Lennard Fisk Lennard Fisk University.

Valentina Abramenko 1, Vasyl Yurchyshyn 1, Philip R. Goode 1, Vincenzo Carbone 2, Robert Stein Big Bear Solar Observatory of NJIT, USA; 2 – Univ.

Evolutionary Characteristics of Magnetic Helicity Injection in Active Regions Hyewon Jeong and Jongchul Chae Seoul National University, Korea 2. Data and.

New Insights into the Sun’s Photosphere Dynamics Offered by New Solar Telescope of BBSO Big Bear Solar Observatory Valentina Abramenko, Vasyl Yurchyshyn,

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

X Visit For 100’s of free powerpoints.

Shock heating by Fast/Slow MHD waves along plasma loops

Anemone Structure of AR NOAA and Related Geo-Effective Flares and CMEs A. Asai 1 ( 浅井歩 ), T.T. Ishii 2, K. Shibata 2, N. Gopalswamy 3 1: Nobeyama.

Introduction to Space Weather Jie Zhang CSI 662 / PHYS 660 Spring, 2012 Copyright © The Sun: Magnetic Structure Feb. 16, 2012.

Scientific rationale for vector polarimetry aboard SDO Or Why do we need to determine photospheric vector fields? Hector Socas-Navarro.

Solar Magnetism: Solar Cycle Solar Dynamo Coronal Magnetic Field CSI 662 / ASTR 769 Lect. 03, February 6 Spring 2007 References: NASA/MSFC Solar Physics.

BBSO 2007 Science Planning. Focal Plane Instruments AO (Wenda, Nicolas, Deqing, Patricia and Park) AO (Wenda, Nicolas, Deqing, Patricia and Park) IRIM.

STOCHASTIC COUPLING OF SOLAR PHOTOSPHERE AND CORONA (Astrophysical J

Diagnostic of Chromospheric Flare Plasma

The Sun: Portrait of a G2V star

The Solar Atmosphere II

Anemone Structure of AR NOAA and Related Geo-Effective Flares and CMEs

Introduction to Space Weather

SIDC Space Weather Briefing

Emerging Active Regions: turbulent state in the photosphere

SIDC Space Weather Briefing

Big Bear Solar Observatory of NJIT

Valentina Abramenko and Kwangsu Ahn

Presentation transcript:

Magnetic fields in the photosphere and heliosphere: structure, statistical parameters, turbulent state Valentyna I. Abramenko Big Bear Solar Observatory of NJIT

Outlook Analysis of line-of-sight magnetograms: - Magnetic energy dissipation structures - Magnetic power spectrum: flare productivity forecast Analysis of the parameters of coronal holes: - Dipole emergence rate in coronal holes - Magnetic Power Spectrum: expansion into the heliosphere Distributions of the magnetic field discontinuities in the solar wind ACE data

Magnetic energy dissipation structures  Abramenko, Yurchyshyn, Wang H., Spirock, Goode 2003, ApJ 597

Coronal Heating High magnetic energy dissipation rate in the photosphere is associated with high temperature and emission measure in the corona. Abramenko, Pevtsov, Romano 2006 ApJ 646

Magnetic Power Spectrum: Flare-quiet active region 0061Flaring active region 9077

PS(corrected) = PS(Full Disk) / Correction Function Correction Function = PS (Full Disk) / PS (High Res)

Emerging Active Region 0488 The power index peaked by the end of the first day of AR’s life, while the magnetic flux has saturated by the end of the 3 rd day flarecontaminatedmeasurements 15h

Soft X-ray Flare Index versus Magnetic power index Abramenko 2005, ApJ, 629

Further study of photospheric magnetograms Separate study of emerging ARs Power spectrum from magnetograms obtained with SDO and Solar B ( possibility for extension of the inertial range, for study of the dissipation range?) Power spectra from different areas on the Sun (ARs, plage areas, Quiet Sun areas, CHs) Structure Functions and Filling Factor in different areas on the Sun

Collaborations in frameworks of the Heliospheric Focus Team Study of the magnetic field parameters inside coronal holes (collaboration with L.A.Fisk and T. Zurbuchen) Analysis of the statistical parameters of the solar wind data (collaboration with B.Vasquez and D.Haggerty)

The Rate of Emergence of Magnetic Dipoles in Coronal Holes and Outside

In all cases, the dipole emerging rate for CHs is lower than that for adjacent QS areas (all data points are above the bisector). This implies that a coronal hole is a region with a local minimum in the rate of emerging dipoles

This result supports the concept that reconnection of open field lines with coronal loops is an important transport mechanism on the Sun (Fisk 2005), and needs to be included in models for the evolution of the solar magnetic field. The dipole emergence rate in Quiet-Sun areas exceeds approximately twice that in Coronal Holes. This implies that a coronal hole is a region with a local minimum in the rate of emerging dipoles.