Optische Sonnenphysik

Präsentation zum Thema: "Optische Sonnenphysik"—  Präsentation transkript:

1 Optische Sonnenphysik
Gruppentreffen am 2. Oktober 2007

2 Astrophysikalisches Institut Potsdam
Agenda Bericht über den 5th Solar Polarization Workshop in Ascona, Schweiz (Horst & Thorsten) DFG Antrag Hochauflösende Beobachtungen von Geschwindigkeitsfeldern in Sonnenflecken und deren Umgebung (Carsten) ERC Advanced Investigator Grant (Carsten) Organisatorisches 13. November 2018 Astrophysikalisches Institut Potsdam

3 5th Polarisation Workshop
Worskshop in honor of Jan Stenflo Discovery of 2nd solar spectrum Sunspot observations not major topic First results of Hinode, problems with the narrow-band imager Polarized radiative transfer, polarization scattering, Hanle effect  no diagnostices, yet 3D radiative transfer is important (H. Uitenbroek) LOS effect of net circular polarization (D. Müller), Hinode sees NCP on fine scale Connection between photospheric and chromospheric magnetic fields 13. November 2018 Astrophysikalisches Institut Potsdam

4 Astrophysikalisches Institut Potsdam
DFG Antrag Zusammenarbeit mit Debi Prasad Choudhary California State University Northridge (CSUN) Ana Cristina Cadavid & Na Deng (CSUN); Chang Liu (BBSO); Thomas Rimmele, Alexandra Tritschler & Friedrich Wöger (NSO/SP) 1 AIP Postdoktorand & Reisegelder 3 Jahre Projektdauer Debi beantragt zusätzliche Gelder (Reisemittel) für sein NSF CAREER Grant Magnetic Tomography of Emerging Sunspots Gemeinsame Beobachtungsaufenthalte (Teneriffa, BBSO & NSO/SP) Jährliche Arbeitsgruppentreffen am AIP und CSUN Internationale Treffen (AAS Solar Physics Division, Fort Lauderdale, Florida, 2008; IAU Symposium No. 259: Cosmic Magnetic Fields, Puerto Santiago, Tenerife, 2008; American Astrophysical Society, Pasadena, California, 2009) Zweidimensionale Spektropolarimetrie (Göttinger FPI, IBIS & VIM) 13. November 2018 Astrophysikalisches Institut Potsdam

5 Astrophysikalisches Institut Potsdam
Science Cases Flow Fields Associated with the Decay of Sunspots On the Relation between Moving Magnetic Features, Evershed Flow, and Sunspot Moat Rapid Decay of Sunspot Penumbrae after Solar Flares Photospheric Shear Flows and the Evolution of Magnetic Shear along Magnetic Neutral Lines in Flaring Active Regions 13. November 2018 Astrophysikalisches Institut Potsdam

6 Astrophysikalisches Institut Potsdam
Penumbral Decay 13. November 2018 Astrophysikalisches Institut Potsdam

7 Penumbral Decay (cont.)
13. November 2018 Astrophysikalisches Institut Potsdam

8 Astrophysikalisches Institut Potsdam
Decaying Sunspot 13. November 2018 Astrophysikalisches Institut Potsdam

9 Horizontal Proper Motions
Local correlation tracking (LCT) for horizontal flow fields in combination with spectroscopy provides 3D photospheric flow field. 13. November 2018 Astrophysikalisches Institut Potsdam

10 3D Magnetic Field Topology
Vector magnetograms provide photospheric boundary conditions for magnetic field extrapolations, which can be compared with chromospheric and coronal loop structures. 13. November 2018 Astrophysikalisches Institut Potsdam

11 Astrophysikalisches Institut Potsdam
Science Goals Identify localized changes of magneto-convection during penumbra formation, i.e., the coupling between the turbulent convective motion and the magnetic field from photosphere and chromosphere, throughout the transition region, and finally the corona. Determine the importance of the local environment, such as filigree and magnetic knots, emerging flux in form of elongated dark channels, or pre-existing photospheric flow fields, for penumbra formation. High-spatial resolution observations provide access to the three-dimensional flow fields in flaring active regions. We will quantify changes in the (shear) flows along their magnetic neutral lines. Are these flows always associated with flux emergence, and in particular, with the magnetic channel structure? Are flows unusually strong before major flares? Do flaring active regions always show complicated flows? Are these flows always associated with flux emergence? Does a correlation between shear flows and major flares exist? What happens to individual penumbral filaments when a segment of the penumbra suddenly disappears during a flare? How does the three-dimensional magnetic field change in the decaying penumbral and strengthening umbral regions? Derive the magnetic helicity injection rate, which is the key to understand the initiation of flares, filament eruptions, and CMEs based on high-resolution observations of three-dimensional flow and magnetic fields in flare/CME source regions. Enhance the understanding of, and predictive capabilities for, solar disturbances that propagate to the Earth. Advance our physical understanding and predictive capabilities for solar driven geo-effective events. 13. November 2018 Astrophysikalisches Institut Potsdam

12 ERC Advanced Investigator Grant
Investigator-Initiated Frontier Research Hauptauswahlkriterium: wissenschaftliche Exzellenz (Kandidatenprofil und Institution) 5 Jahre, €100k – €500k pro Jahr Frist ist wahrscheinlich Ende des Jahres PI Projekt (kein Netzwerk) Aufbau einer Gruppe Zweistufiges Begutachtungsverfahren CV und Selbsteinschäzung (3 Seiten), Projektbeschreibung (4 Seiten) und Institution (1 Seite) Unsere Themen: Entwicklung eines “blauen” FPIs für GREGOR und ein 30-cm photometrisches Sonnenteleskop (blaues Kontinuum, G-Band und Ca II K) für die Antarktis Pilotprojekt für ein zwei-dimensionales Spektropolarimeter in der Antarktis 13. November 2018 Astrophysikalisches Institut Potsdam

13 Astrophysikalisches Institut Potsdam
Organisatorisches WWW Auftritt 16. Oktober: 6. November: 20. November: 4. Dezember: 18. Dezember: 13. November 2018 Astrophysikalisches Institut Potsdam