Space weather at University of Graz / Kanzelhöhe Observatory Institute of Physics, University of Graz, Austria Kanzelhöhe Observatory, Gerlitzen (Austria)

Slides:

Advertisements

Similar presentations

Use of the Frequency Agile Solar Radiotelescope for Space Weather A New Solar-dedicated Radio Facility Dale E. Gary, NJIT; Stephen M. White, U Maryland.

Advertisements

Space Weather User Needs Related to Solar Observations Eamonn Daly and Alexi Glover ESA Space Environments and Effects Section ESTEC, The Netherlands.

Evolution of Magnetic Setting in Flare Productive Active Regions Yixuan Li Space Weather Research Lab New Jersey Institute of Technology.

Splinter: SSA Space Weather Service Network Splinter: SSA Space Weather Service Network Tuesday 18th, 15: :00 1.Overview of the P2-SSA activities.

PARTS V: GEOMAGNETIC INDICES Observed, estimated, and predicted daily geomagnetic AFr-indices (A- indices from Fredericksburg, VA), and daily AP-indices.

Real-Time Reconstructions of the Solar Irradiance for Space Weather Applications in the SOTERIA Project Framework 7th European Space Weather Week, November.

11/26/081 AUTOMATIC SOLAR ACTIVITY DETECTION BASED ON IMAGES FROM HSOS NAOC, HSOS YANG Xiao, LIN GangHua

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.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

ASSA (Automatic Solar Synoptic Analyzer) Sunhak Hong 1,2, Sangwoo Lee 3, Seung Jun Oh 3, Jae Hun Kim 1, Gi-Chang Yoon 1, Jae-Hyung Lee 1,2, Young-Kyu Kim.

High Altitude Observatory (HAO) – National Center for Atmospheric Research (NCAR) The National Center for Atmospheric Research is operated by the University.

E. Robbrecht – SIDC- Royal Observatory of Belgium 8 March 2007 The statistical importance of narrow CMEs Open questions to be addressed by SECCHI Eva Robbrecht,

2010 March 10 Current status of GHN and fast-mode flare observations Yan Xu SWRL/NJIT.

HMI – Synoptic Data Sets HMI Team Meeting Jan. 26, 2005 Stanford, CA.

Big Bear Solar Observatory / NJIT Active Region Monitor (ARM;  A web-based summary of the latest solar activity (every hour update)

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

Discussion Summary: Group B –Solar Active Regions And Their Production of Flares and Coronal Mass Ejections Discussion Leaders: George Fisher Hugh Hudson.

Solar Activities and Halloween Storms Ahmed Hady Astronomy Department Cairo University, Egypt.

Magnetic Shear in Two-ribbon Solar Flares Yingna Su 1,2 Advisors: Leon Golub 1, Guangli Huang 2 Collaborators: A. A. Van Ballegooijen 1, E. E. Deluca 1,

Coronal Ejecta in October - November of 2003 and predictions of the associated geomagnetic events 1 Big Bear Solar Observatory, New Jersey Institute of.

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

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

Connecting coronal structure to photospheric origins Active region (sunspot) evolution and solar rotation well define long term, persistent, coronal streamers.

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

Sung-Hong Park Space Weather Research Laboratory New Jersey Institute of Technology Study of Magnetic Helicity and Its Relationship with Solar Activities:

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

PROBA2 a Space Weather Monitor Matthew J West ESWW10 - Nov 2013.

Science Data Products – HMI Magnetic Field Images Pipeline 45-second Magnetic line-of-sight velocity on full disk Continuum intensity on full disk Vlos.

History of Hvar double solar telescope Installed in 1972 based on an agreement between Faculty of Geodesy of the University of Zagreb and the Astronomical.

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

The Dangers of Solar Storms and Solar Cycles.  For every 1 million atoms of hydrogen in the entire sun  98,000 atoms of helium  850 of oxygen  360.

High-Cadence EUV Imaging, Radio, and In-Situ Observations of Coronal Shocks and Energetic Particles: Implications for Particle Acceleration K. A. Kozarev.

Digitization in Kodaikanal Observatory References and useful links :

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.

Collaboration of BBSO/NST and SOT Haimin Wang Big Bear Solar Observatory 1. Six-station Global Full Disk Halpha Network –Large scale structure of flares.

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

- “Level” refers to the long-term irradiance, measured as the significant daily minimum, i.e. without flares or instrumental artefacts. - “Variance” refers.

Development of space weather in Japan Hiroaki Isobe Center for the Promotion of Interdisciplinary Education and Research Kyoto University.

The day after solar cycle 23 IHY 2009 September 23, 2009 Yu Yi 1 and Su Yeon Oh 2 1 Dept. of Astronomy & Space Science, Chungnam National University, Korea.

H.N. Wang Key Laboratory of Solar Activity National Astronomical Observatory Chinese Academy of Sciences SDO data for solar activity forecasts.

Ivana Poljančić Physics Department University of Rijeka, Croatia IHY-ISWI Regional Meeting Heliophysical phenomena and Earth's.

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

Chapter 9 Our Star, the Sun. What do you think? What is the surface of the Sun like? Does the Sun rotate? What makes the Sun shine?

1 Machine Learning and Data Mining for Automatic Detection and Interpretation of Solar Events Jie Zhang (Presenting, Co-I, SCS*) Art Poland (PI, SCS*)

OBSERVING THE SUN & PLANETARY TRANSITS Petr HEINZEL Solar Physics Department Astronomical Institute of the Academy of Sciences Czech Republic.

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

Direct Spatial Association of an X-Ray Flare with the Eruption of a Solar Quiescent Filament Gordon D. Holman and Adi Foord （２０１５） Solar Seminar on July.

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.

SOLAR DEMON DETECTING FLARES, DIMMINGS, AND EUV WAVES IN NEAR REAL-TIME ON SDO/AIA IMAGES Emil Kraaikamp (p), Cis Verbeeck – Royal Observatory of Belgium.

ITT: SEP forecasting Mike Marsh. Solar radiation storms Solar energetic particles (SEPs)

The Helioseismic and Magnetic Imager (HMI) on NASA’s Solar Dynamics Observatory (SDO) has continuously measured the vector magnetic field, intensity, and.

Solar X-ray Imager (SXI) Current and Future Requirements 22 May 2001 Steve Hill Solar Causes and Effects... Operational Requirements Improvements for GOES-R+

Multi-Point Observations of The Solar Corona for Space weather Acknowledgements The forecasting data was retrieved from NOAA SWPC products and SIDC PRESTO.

The CME geomagnetic forecast tool (CGFT) M. Dumbović 1, A. Devos 2, L. Rodriguez 2, B. Vršnak 1, E. Kraaikamp 2, B. Bourgoignie 2, J. Čalogović 1 1 Hvar.

Space Weather Service in Indonesia Clara Y. Yatini National Institute of Aeronautics and Space (LAPAN)

Arnold Hanslmeier Institut f. Physik Universität Graz, Austria.

ESSEM Earth System Science and Environmental Management 17/11/ ESWW6-2 M. Messerotti, A. Marassi M. MESSEROTTI 1,2,3, A. MARASSI 1 1 INAF-Astronomical.

CME – Flare Relationship A survey combining STEREO and RHESSI observations S. Berkebile-Stoiser B. Bein A.Veronig M. Temmer.

Digitization in Kodaikanal Observatory

On behalf of the ARGO-YBJ collaboration

Studies on Twisted Magnetic Flux Bundles

“Old” data – new science or why do we need long-term synoptic programs

GONG Measurements – Pre-eruptive signatures

WG2: Magnetographs and solar-disk white-light imagers

Hiroko Watanabe (Kyoto Univ.)

HMI Data Analysis Pipeline

HMI Data Analysis Pipeline

Ju Jing, Vasyl B. Yurchyshyn, Guo Yang, Yan Xu, and Haimin Wang

Solar Activity Forecast for the Next Decade

SIDC Space Weather Briefing

Presentation transcript:

Space weather at University of Graz / Kanzelhöhe Observatory Institute of Physics, University of Graz, Austria Kanzelhöhe Observatory, Gerlitzen For more details Pötzi et al., 2014

Location: Gerlitzen (Carinthia) ~1500m a.s.l. Kanzelhöhe Observatory (KSO) is an ESA-Expert Service Center for Solar Weather, RWC of ISES, and valuable partner within several international networks for ground based observations. Ground based observations at the Kanzelhöhe Observatory in Austria Patrol observations of the Sun for Space Weather (prediction): Active regions containing sunspots: white-light data Solar flares: H-alpha data ~70% of CMEs are associated with erupting filaments: H-alpha data Impulsive flares and CMEs are rooted in the strong magnetic fields of sunspots: Ca II K data (magnetic field proxy)

Data products relevant for Space Weather Full disk images are derived 7 days a week (if weather permits). Data are available in near real-time. Maximum latency < 5 min. Images of class 1 quality are immediately processed providing real-time flare and filament eruption alerts. 4 MegaPixel 12 bit 10 images / minute Filaments Flares Plages Sunspots 4 MegaPixel 12 bit 10 images / minute 4 MegaPixel 10 bit 1 image / minute H-alpha Ca II K White-light

Real-time flare detection and ESA alerts Detection of flare occurrence, heliographic location, time and size of the flare at maximum intensity. Real-time provision of a flare importance class (optical) based on these parameters. Alert will be issued when a flare is detected and exceeds a certain strength in terms of area and intensity (Importance ≥1).

Real-time filament detection (beta-version) ~ 8 images processed / min the delay time for an alert is ~ 1 min. L_18 eruption: fragments of filaments 2 → 1 3 → 3

High cadence data (time cadence of up to 6 seconds during flare events) KSO online archive: synoptic and high-cadence data Overview of daily observations, free and user-friendly access to all scientific data, through KSO website.