1 A Statistical Study about Transequatorial loops Jie Chen National Astronomical Observatories Chinese Academy of Sciences.

Slides:



Advertisements
Similar presentations
Vu Pham A new dynamo pattern revealed by the tilt angle of bipolar sunspot groups Egor Illarionov Moscow State University Helicity Thinkshop on Solar Physics.
Advertisements

2011/08/ ILWS Science Workshop1 Solar cycle prediction using dynamos and its implication for the solar cycle Jie Jiang National Astronomical Observatories,
Sunspots and the Scientific Method: Models. Hypothesis Driven Science Hypothesis: An educated speculation about how a particular phenomenon behaves- very.
Estimating the magnetic energy in solar magnetic configurations Stéphane Régnier Reconnection seminar on Thursday 15 December 2005.
H.N. Wang 1 , H. He 1, X. Huang 1, Z. L. Du 1 L. Y. Zhang 1 and Y. M. Cui 2 L. Y. Zhang 1 and Y. M. Cui 2 1 National Astronomical Observatories 2 National.
An overview of the cycle variations in the solar corona Louise Harra UCL Department of Space and Climate Physics Mullard Space Science.
Evolution of Barb-Angle and Partial Filament Eruption J.T. Su [1,2], Y. Liu [2], H.Q. Zhang [1], H. Kurokawa [2] V. Yurchyshyn [3] (1)National Astronomical.
Reviewing the Summer School Solar Labs Nicholas Gross.
The Relation between Filament Skew Angle and Magnetic Helicity of Active Regions Masaoki HAGINO, Y.J. MOON (Korea Astronomy and Space Science Institute)
Jonathan A. Constable University of St Andrews Solar REU Presentation 2009 A flux rope model for CME initiation over solar cycle 23 Jonathan Constable.
AGU – Fall 2006 The Solar Polar Field – Cycles 21 – 23 The Solar Polar Field During Solar Cycles J. Todd Hoeksema, Yang Liu, XuePu Zhao & Elena Benevolenskaya.
High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.
State Key Laboratory of Space Weather An inter-hemisphere asymmetry of the cusp region against the geomagnetic dipole tilt Jiankui Shi Center for Space.
Rapid Changes in the Longitudinal Magnetic Field Associated with the July gamma -ray Flare Vasyl Yurchyshyn, Haimin Wang, Valentyna Abramenko,
The May 1,1998 and May 12, 1997 MURI events George H. Fisher UC Berkeley.
Working Group E: The Pre-CME Sun - Pre-eruption structure, evolution & energy release - Global issues: helicity, homologous CMEs - Inputs to CME initiation.
Accurate Polar and small scale observations during the solar cycle Elena E. Benevolenskaya Yang Liu J. Todd Hoeksema Stanford University HMI/AIA meeting,
Absence of a Long Lasting Southward Displacement of the HCS Near the Minimum Preceding Solar Cycle 24 X. P. Zhao, J. T. Hoeksema and P. H. Scherrer Stanford.
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.
EUV vs. B-field Comparisons Yingna Su Smithsonian Astrophysical Observatory Coauthours: Leon Golub, Aad Van Ballegooijen, Maurice Gros. HMI/AIA Science.
SPD – June 2006 Solar Polar Flux – MDI The Sun’s Polar Magnetic Flux Observed with SOHO/MDI J. Todd Hoeksema E.E. Benevolenskaya,
Sung-Hong Park Space Weather Research Laboratory New Jersey Institute of Technology Study of Magnetic Helicity and Its Relationship with Solar Activities:
The May 1997 and May 1998 MURI events George H. Fisher UC Berkeley.
What stellar properties can be learnt from planetary transits Adriana Válio Roque da Silva CRAAM/Mackenzie.
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.
Statistical properties of current helicity and twist distribution in the solar cycle by high resolution data from SOT/SP on board Hinode K. Otsuji 1),
Comparison on Calculated Helicity Parameters at Different Observing Sites Haiqing Xu (NAOC) Collaborators: Hongqi, Zhang, NAOC Kirill Kuzanyan, IZMIRAN,
Quick changes of photospheric magnetic field during flare-associated surges Leping Li, Huadong Chen, Suli Ma, Yunchun Jiang National Astronomical Observatory/Yunnan.
1 Mei Zhang ( National Astronomical Observatory, Chinese Academy of Sciences ) Helicity Transport from the convection zone to interplanetary space Collaborators:
Coronal Mass Ejection As a Result of Magnetic Helicity Accumulation
Study of Local Heliospheric Current Sheet Variations from Multi-Spacecraft Observations D. Arrazola · J.J. Blanco · J. Rodríguez-Pacheco · M.A. Hidalgo.
1 THE RELATION BETWEEN CORONAL EIT WAVE AND MAGNETIC CONFIGURATION Speakers: Xin Chen
Helicity Observations by Huairou Vector Magnetograph Mei Zhang National Astronomical Observatory, Chinese Academy of Sciences Plan of the Talk: 1.Huairou.
Propagation Trends Dayton 2014 Solar Maximum! But the slow decline to solar minimum in 2020 is likely to begin later this year.
Solar Maximum ! A Double Peaked Sunspot Cycle ?
NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.
ASAI Ayumi Kwasan Observatory, Kyoto University July 12, Evolution of Flare Ribbons and Energy Release.
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.
The Rise of Solar Cycle 24: Magnetic Fields from the Dynamo through the Photosphere and Corona and Connecting to the Heliosphere Part 2: Corona & Heliophere.
1 Mei Zhang ( National Astronomical Observatory, Chinese Academy of Sciences ) Solar cycle variation of kinetic helicity Collaborators: Junwei Zhao (Stanford,
Негауссовские распределения спиральности солнечных магнитных полей в цикле активности Kuzanyan Kirill Kuzanyan Kirill; Sokoloff Dmitry (IZMIRAN, RAS &
1 Yongliang Song & Mei Zhang (National Astronomical Observatory of China) The effect of non-radial magnetic field on measuring helicity transfer rate.
Moving Magnetic Features (MMFs) Jun Zhang National Astronomical Observatories Chinese Academy of Sciences Collaborators: Sami Solanki and Jingxiu Wang.
ИЗМЕНЕНИЯ МАГНИТНОЙ СПИРАЛЬНОСТИ В СОЛНЕЧНОМ ЦИКЛЕ Kirill Kuzanyan ИЗМИРАН, Россия Zhang H., Gao Yu Национальные Астрономические Обсерватории АН КНР.
Sunspot activity and reversal of polar fields in the current cycle 24 A.V. Mordvinov 1, A.A. Pevtsov 2 1 Institute of Solar-Terrestrial Physics of SB RAS,
What the Long-Term Sunspot Record Tells Us About Space Climate David H. Hathaway NASA/MSFC National Space Science and Technology Center Huntsville, AL,
Monday Seminar Talk (short) 17 November, 2003 Taro Morimoto.
1 NSSC National Space Science Center, Chinese academy of Sciences FACs connecting the Ionosphere and Magnetosphere: Cluster and Double Star Observations.
Helicity Thinkshop 2009, Beijing Asymmetry of helicity injection in emerging active regions L. Tian, D. Alexander Rice University, USA Y. Liu Yunnan Astronomical.
CMEs: Taking magnetic helicity from low corona
On the three-dimensional configuration of coronal mass ejections
Review Question Why does the Sun shine?.
Estimates of the forthcoming solar cycles 24 and 25
Introduction to Space Weather
Overview of the Sun Jie Zhang Art Poland
Anemone Structure of AR NOAA and Related Geo-Effective Flares and CMEs
­Long-Term Variation of Latitudinal Distribution of Coronal Holes
Solar and Heliospheric Physics
Preflare State Rust et al. (1994) 太陽雑誌会.
Flare Ribbon Expansion and Energy Release
Ju Jing, Vasyl B. Yurchyshyn, Guo Yang, Yan Xu, and Haimin Wang
Ron Moore and Alphonse Sterling
Imaginary Lines on a Map
Magnetic Helicity In Emerging Active Regions: A Statistical Study
Sushanta C. Tripathy National Solar Observatory
A Presentation to the SHINE ’02 Workshop by J.G. Luhmann
Closing the Books on Cycle 24 J
Presentation transcript:

1 A Statistical Study about Transequatorial loops Jie Chen National Astronomical Observatories Chinese Academy of Sciences

2 Transequatorial Loops(TELs) have relation to some solar physics phenomena They may be relevant to solar dynamo model (Babcock,1961) The evolution of TELs reflects magnetic reconnection (Tsuneta, 1996) The disappearance or brighten of TELs has relation to CME or flare eruption (Khan et al.2000; Glover et al.) Active regions which have the same chirality are more easily to form TELs (Canfield et al.1996; Farnik et al.1999; Pevtsov 2000)

3 Our Work Data Base and Observation Whole YOHKOH/SXT data set (1991 October December) SOHO/MDI and Kitt Peak full disk longitude magnetograms We choose the images which are most clear and close to the middle of solar disk Find 356 TELs

4 Category According to the magnetic polarities that TELs connect the regions in photosphere: PTEL, FTEL PTEL SPTEL FTEL SFTEL

5 According to the numbers of TELs that the same region connected and magnetic polarities, we can classify TELs to SPTEL, SFTEL; DTELsA, DTELsB, DTELsC DTELsA DTELsB DTELsC

6 TEL (number)356100% PTEL22964% FTEL12736% TEL CLASSIFICATION STELDTELs SPTELSFTELDTELsADTELsBDTELsC %21%71%20%9% %57% Statistical Results

7 Discussion About bipolar group, the leading polarity is more compact and lives longer than the following polarity, the preceding polarity is more easy to form TELs than the following polarity, so PTEL has a larger proportion than FTEL When the two active regions both are mature, then the following polarity has the same probability with the leading polarity, so DTELsA has a larger ratio

8 solar cycle 22 TEL148100% PTEL9161% FTEL5739% solar cycle 23 TEL208100% PTEL13866% FTEL7034% Preference Independent of Solar Cycle During solar cycle 22, in the northern hemisphere, the leading polarity is negative; during solar cycle 23, magnetic polarity is reversed

9 A: TELs number in different years B: the percent is TELs to sunspot number C: PTEL number in different years D: FTEL number in different years TELs number has the same trend with solar cycle The ratio of TELs to sunspot number is about 10%

10 Some Parameters about TELs Separation: the footpoints distance between regions that TELs connected (Chase et al.,1977; Farnik et al.1999; Pevtsov, 2000 &2004) Tilt Angle: the angle between TELs and equator ( Pevtsov 2004 ) Asymmetry in Latitude: the footpoints asymmetry in latitude of TELs These parameters reflect the properties of TELs and maybe have relation with solar dynamo Through compute flux-weighted center of the magnetic polarities, we calculate these parameters

11 Separation Mean value is about 27 0 ( similar to Pevtsov(2000) result) It decreases from the minimum of solar cycle to maximum, this result is consistent to radial magnetic field variation following solar cycle

12 Tilt angle When the north footpoint is to the west of south footpoint, the angle is less than 90 0 ; reverse, it is more than 90 0 Mean value is about 90 0 Tilt angle value in different years

13 Asymmetry in Latitude Mean value is 0.6 Asymmetry in latitude is different in different years If the latitude value in northern hemisphere is larger than it is in southern hemisphere, the result is more than 0; reverse, it is less than 0

14 separation tilt angle asymmetry in latitude total average solar cycle solar cycle Three Parameters are All Different in Different Solar Cycle

15 Result 1.About TELs, PTEL has a preference and this result is independent of solar cycle 2.TELs number variation following solar cycle and the ratio of TELs to sunspot number is about 10% 3. Separation, Tilt Angle, Asymmetry in Latitude is different in different solar cycle

16 Thank you!