19:30 Lobby Self-paid dinner in a nearby restaurant. Comparing and Validating Meridional Flow Derivations in the Solar Convection Zone
|
|
|
- Valerie Poole
- 6 years ago
- Views:
Transcription
1 Conference Programme Sunday - August 30, :00 20:00 Lobby Registration 18:30 Lobby City Tour 19:30 Lobby Self-paid dinner in a nearby restaurant Monday - August 31, :00 Foyer Registration (whole week) 9:30 12:20 Room "Colmar" Splinter I: Comparing and Validating Meridional Flow Derivations in the Solar Convection Zone 09:25-12:30 Conference Room "Basel" Splinter II: Waves inside Stars: Theory, Simulations, Observational Signatures, and Lab Experiments 10:30 11:00 Coffee Break & Posters 12:30 14:00 Lunch at Restaurant La Rotonde Session I: Solar and Stellar Observations Chair: Frank Hill 14:00 Markus Roth Welcome 14:10 Lucia Kleint Invited Talk: An Overview of Polarimetry 14:40 Roman Brajsa Modeling Radiation from the Solar Atmosphere in the sub-mm, mm and cm Wavelength Range 15:00 Christopher J. Nelson On The Relationship Between Ellerman Bombs and Other Solar Processes
2 15:20 Jan Langfellner Anisotropy of the solar network magnetic field around the average supergranule 15:40 16:10 Coffee Break & Posters 16:10 Manfred Schüssler The cause of the weak solar cycle 24 16:30 Rob Rutten A new view of the Halpha chromosphere 16:50 Sanjay Gosain Full Stokes Polarimeter for Chromospheric Measurements with SOLIS/VSM 17:10 Junwei Zhao Establishing Connections between Photospheric Waves and Coronal Waves in Active Regions 17:30 Sanjay Gosain A Proposal for Next Generation Synoptic Solar Instrumentation 17:50 Frank Hill GONG Status Tuesday - September 1, 2015 Session II: Solar and Stellar Modelling Chair: Rudi Komm 09:00 Matt Browning Invited Talk: Global Simulations of solar and stellar dynamos: cycles, theories, and limits 09:30 Manfred Schüssler The Babcock-Leighton solar dynamo 09:50 Jacobo Varela Differential Rotation and Dynamo Action in Solar-like Stars 10:10 Zarzalt Magic Inivted Talk: 3D MHD Stellar Atmosphere Simulations 10:40 11:10 Coffee Break & Posters 11:10 Laurene Jouve Invited Talk: Models and data combined to progress towards a better understanding of the magnetism of solar-type stars 11:40 Volkmar Holzwarth Joint magnetospheres of close "solar-twin" binary systems
3 12:00 Aditi Sood Dynamical model for spindown of solar-type stars 12:20 Conference Photo 12:30 14:00 Lunch at Restaurant La Rotonde Session III: Solar and Stellar Seismology Chair: John Leibacher 14:00 Ariane Schad Invited Talk: Global helioseismic measurement of meridional circulation and differential rotation from mode eigenfunction perturbations 14:30 S.P. Rajaguru Deep structure of solar meridional circulation: helioseismic inferences from four years of HMI/SDO observations 14:50 Ruizhu Chen Measurement of deep solar meridional flow and its temporal variation 15:10 Dean-Yi Chou Solar-Cycle Variations of Meridional Flows and Magnetic Signature at the Base of Convection Zone 15:30 Rosaria Simoniello Helioseismic Signatures of the Progression of Solar Cycle: A Reflection of a Dynamo Wave 15:50 16:20 Coffee Break & Posters 16:20 Charles S. Baldner Variations in Large-scale Flow Structures in the Current Solar Cycle 16:40 Rudolf Komm Large-scale subsurface flows during Solar Cycle 23 and 24 17:00 Anne-Marie Broomhall Statistical searches for low signal-to-noise oscillations 17:20 Kaori Nagashima Measurement of the amplitude of the solar cross-covariance function 17:40 Vincent Böning Validating Spherical Born Kernels for Meridional Flows 18:00 Björn Löptien Data Compression for Helioseismology
4 Wednesday - September 2, 2015 Session III: Solar and Stellar Seismology (continued) Chair: Rekha Jain 09:00 Damien Przybylski Signatures of mode conversion in a sunspot simulation 09:20 Khalil Daiffallah Helioseismology of sunspot models 09:40 Rudolf Komm Subsurface helicity of active regions and :00 Johannes Löhner-Böttcher Magnetic field reconstruction based on sunspot oscillations 10:20 10:50 Coffee Break & Posters 10:50 Ângela Santos Contribution from sunspots to the observed frequency shifts 11:10 Kiran Jain Response of Solar Oscillations to The Magnetic Activity: Comparison between Solar Cycles 23 and 24 11:30 Jesper Schou What to do Next in Global Mode Seismology? 11:50 Foyer Packed Lunch Excursion to Europa-Park Rust & Conference Dinner 12:45 Buses leave to Rust 13:30 Entry into Europa-Park Rust via the entrance of the Hotel El Andaluz 20:00 23:00 Conference Dinner at Hotel Santa Isabella, Room: Convento 23:00 Buses return to Freiburg
5 Thursday - September 3, 2015 Session III: Solar and Stellar Seismology (continued) Chair: Conny Aerts 09:00 Sarbani Basu Invited Talk: Seismic inferences of solar and stellar structure 09:30 George Angelou On the Utility of Diagrams of Small Frequency vs Large Frequency Separation 09:50 Elisabeth Guggenberger Towards an improvement of the scaling relations 10:10 Mutlu Yildiz Effects of the HeII ionization zones on oscillation frequencies and their promises 10:30 11:00 Coffee Break & Posters 11:00 Maria Bergemann Invited Talk: Chemical abundances of the Sun and solar-like stars 11:30 Vincent Ballenegger Thermodynamic properties of hydrogen and hydrogen-helium mixtures under solar conditions 11:50 Antonio Ferriz-Mas Chandrasekhar's adiabatic exponents and other material coefficients for stellar interiors 12:10 Ehsan Moravveji Tight asteroseismic constraints on core overshooting and diffusive mixing for massive stars 12:30 Gaël Buldgen Constraining mixing processes in 16CygA and 16CygB using Kepler data and seismic inversion 12:50 14:15 Lunch at Restaurant La Rotonde Session IV: In Memory of Jean-Paul Zahn Chair: Eric Michel 14:15 Stephane Mathis / Ian Roxburgh Invited Talk: A Tribute to Jean-Paul Zahn 14:45 Sebastien Deheuvels Invited Talk: What asteroseismology is teaching us about the internal rotation of stars 15:15 Santiago Andres Triana The internal rotation of stars as revealed by asteroseismic inversions 15:35 16:15 Coffee Break & Posters
6 16:15 Vincent Prat Ray dynamics of gravito-inertial modes in rapidly rotating stars 16:35 Paul G. Beck Seismic analysis of red giant stars in binary systems the heartbeat of red giants 16:55 Wiebke Herzberg The effect of large scale flows on the eigenfrequencies of subgiant stars 17:15 Guy Davis Invited Talk: Sounding solar and stellar activity cycles using asteroseismology Friday - September 4, 2015 Session V: Solar and Stellar Activity Chair: Guy Davis 09:00 Thomas Ayres Invited Talk: The Ups and Downs of Stellar Activity 09:30 Svetlana Berdyugina Invited Talk: Overview on sunspots and starspots 10:00 Lousie Harra Invited Talk: Review of solar flares 10:30 11:00 Coffee Break & Posters 11:00 Ralph Neuhäuser Strong variations of 14-C around AD 775 and AD due to solar activity 11:20 Manfred Kitze Superflares on solar analogue stars 11:40 Rekha Jain Oscillations in a solar coronal arcade near a flare-site 12:00 Alina Donea Invited Talk: Seismicity induced by solar and stellar flares: comparison 12:30 Frederic Baudin Flares and solar p-modes 12:50 Goodbye 13:00 14:00 Lunch at Restaurant La Rotonde 14:00 Conference Room "Basel" left Splinter III: Open-access tools for local helioseismology provided by SpaceInn
7 14:00 Conference Room "Basel" right Splinter IV: Meridional flow, α effect, single vs multiple dynamo: addressing open issues in solar/stellar dynamo with p-mode parameters 15:30 16:00 Coffee Break 17:00 End
FThalr Twitter: #cid_solarnet3_2015 ScienceMedia CID: solarnet3.2015
FThalr Twitter: #cid_solarnet3_2015 ScienceMedia CID: solarnet3.2015 1 Contents Conference Programme... 6 Splinter Sessions... 14 Splinter I: Comparing and Validating Meridional Flow Derivations in the
HELAS VI / SOHO 28 / SPACEINN Helioseismology and Applications
HELAS VI / SOHO 28 / SPACEINN Helioseismology and Applications Programme 1-5 September 2014 G ottingen, Germany Hosted by the Max Planck Institute for Solar System Research Programme Organizing Committee:
5:00pm-8:00pm Ala Moana, Carnation
210th Meeting of the AAS, joint meeting with SPD 27-31 May 2007 - Honolulu, HI Hawaii Convention Center, 1801 Kalakaua Ave., Honolulu, HI 96815 Thursday, May 24, 2007 Endpoints & Interactions: Physics
The Solar Physics Research Integrated Network Group SPRING
The Solar Physics Research Integrated Network Group Markus Roth, Sanjay Gosain, Frank Hill, Michael Thompson European Space Weather Week November 23, 2015 The Need for Synoptic Observations of the Sun
The Solar Interior and Helioseismology
The Solar Interior and Helioseismology Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK STFC Advanced Summer School, 2016 Sep 6 University of Sheffield http://solarscience.msfc.nasa.gov/predict.shtml
Daily agenda & scientific program
Daily agenda & scientific program Sunday June 22, 2014 Welcome reception 16h00-19h00 welcome and registration reception at the Science history museum Villa Bartholoni 128, route de Lausanne 1201 Genève
Status of solar and stellar modelling. Jørgen Christensen-Dalsgaard Stellar Astrophysics Centre Aarhus University
Status of solar and stellar modelling Jørgen Christensen-Dalsgaard Stellar Astrophysics Centre Aarhus University Excellent? Excellent? Probably poor! What kind of models? Model of eclipsing-binary system
The Sun: A Star of Our Own ASTR 2110 Sarazin
The Sun: A Star of Our Own ASTR 2110 Sarazin Sarazin Travel Wednesday, September 19 afternoon Friday, September 21 Will miss class Friday, September 21 TA Molly Finn will be guest lecturer Cancel Office
Solar Structure. Connections between the solar interior and solar activity. Deep roots of solar activity
Deep roots of solar activity Michael Thompson University of Sheffield Sheffield, U.K. michael.thompson@sheffield.ac.uk With thanks to: Alexander Kosovichev, Rudi Komm, Steve Tobias Connections between
AASTCS 5: Radio Exploration of Planetary Habitability 7 12 May, 2017
AASTCS 5: Radio Exploration of Planetary Habitability 7 12 May, 2017 Sunday 7 May, 2017 3:00 pm 7:00 pm 6:00 pm 7:30 pm Registration and Speaker Ready, Tuscany Foyer Opening Reception, Miramonte Green
Logistics 2/14/17. Topics for Today and Thur. Helioseismology: Millions of sound waves available to probe solar interior. ASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Pleiades Star Cluster Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 9 Tues 14 Feb 2017 zeus.colorado.edu/astr1040-toomre Topics for Today and Thur Helioseismology:
Helioseismology. Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK
Helioseismology Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK STFC Advanced Summer School, 2014 Sep 1 University of Dundee http://solarscience.msfc.nasa.gov/predict.shtml http://solarscience.msfc.nasa.gov/predict.shtml
AASTCS 5: Radio Exploration of Planetary Habitability 7 12 May, 2017
AASTCS 5: Radio Exploration of Planetary Habitability 7 12 May, 2017 Sunday 7 May, 2017 3:00 pm 7:00 pm 6:00 pm 7:30 pm Welcome Reception Miramonte Green Monday 8 May, 2017 8:00 am Stellar Activity and
Logistics 2/13/18. Topics for Today and Thur+ Helioseismology: Millions of sound waves available to probe solar interior. ASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Pleiades Star Cluster Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 9 Tues 13 Feb 2018 zeus.colorado.edu/astr1040-toomre Topics for Today and Thur+ Helioseismology:
STELLAR PHYSICS OF THE SOLAR INTERIOR IN THE COMING DECADE
STELLAR PHYSICS OF THE SOLAR INTERIOR IN THE COMING DECADE A Science White Paper for the Astro 2010 Decadal Survey Submitted for consideration by the Stars and Stellar Evolution Panel Frank Hill National
The Sun. The Sun. Bhishek Manek UM-DAE Centre for Excellence in Basic Sciences. May 7, 2016
The Sun Bhishek Manek UM-DAE Centre for Excellence in Basic Sciences May 7, 2016 Outline 1 Motivation 2 Resume of the Sun 3 Structure of the Sun - Solar Interior and Atmosphere 4 Standard Solar Model -
Peak-bagging in Helio- and Astero-seismology
Report of the 1 st SpaceInn Workshop 4.1 March 11-13, 2014 Tenerife, Spain Peak-bagging in Helio- and Astero-seismology SpaceInn Grant Agreement no: 312844 SOC: Dr. A. Eff-Darwich (Ull-IAC), Dr. R.A. García
Helioseismology. Jesper Schou Max Planck Institute for Solar System Research
Helioseismology Jesper Schou Max Planck Institute for Solar System Research schou@mps.mpg.de Page 1 of 60 Helioseismology The study of the Sun using waves Similar to Earth seismology Sounds waves are trapped
2 Solar models: structure, neutrinos and helioseismological properties 8 J.N. Bahcall, S. Basu and M.H. Pinsonneault
Foreword xv E.N. Parker 1 Dynamic Sun: an introduction 1 B.N. Dwivedi 1.1 Introduction 1 1.2 Main contents 2 1.3 Concluding remarks 7 2 Solar models: structure, neutrinos and helioseismological properties
Meridional Flow, Torsional Oscillations, and the Solar Magnetic Cycle
Meridional Flow, Torsional Oscillations, and the Solar Magnetic Cycle David H. Hathaway NASA/MSFC National Space Science and Technology Center Outline 1. Key observational components of the solar magnetic
The Sun Our Extraordinary Ordinary Star
The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the
An Overview of the Details
The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the
An Overview of the Details
Guiding Questions The Sun Our Extraordinary Ordinary Star 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the Sun
Chapter 1. Introduction. 1.1 Motivation
Chapter 1 Introduction 1.1 Motivation The Sun is a fascinating star, which not only supports life on the Earth, but also exhibits some extraordinary scientific phenomena, such as solar flares, coronal
Observed solar frequencies. Observed solar frequencies. Selected (two) topical problems in solar/stellar modelling
Selected (two) topical problems in solar/stellar modelling Stellar Astrophysics Centre Improving solar physics by studying other stars Günter Houdek The effect of the surface layers on the oscillation
9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is
1 9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is produced by the proton-proton chain in which four hydrogen
PTYS/ASTR 206. The Sun 3/1/07
The Announcements Reading Assignment Review and finish reading Chapter 18 Optional reading March 2006 Scientific American: article by Gene Parker titled Shielding Space Travelers http://en.wikipedia.org/wiki/solar_variability
STELLAR ROTATION AND MAGNETIC ACTIVITY:
STELLAR ROTATION AND MAGNETIC ACTIVITY: USING ASTEROSEISMOLOGY Rafael A. García Service d Astrophysique, CEA-Saclay, France Special thanks to: S. Mathur, K. Auguston, J. Ballot, T. Ceillier, T. Metcalfe,
Astronomy 1 Winter 2011
Astronomy 1 Winter 2011 Lecture 19; February 23 2011 Asteroids Comets Meteors Previously on Astro-1 Homework Due 03/02/11 On your own: answer all the review questions in chapters 16 17 and 18 To TAs: answer
Helios in Greek and Sol in Roman
Helios in Greek and Sol in Roman Drove his chariot across the sky to provide daylight Returned each night in a huge golden cup on the river Oceanus His son Phaeton drove the chariot one day but lost control
Local helioseismology: methods and challenges
1 Local helioseismology: methods and challenges Doug Braun contributions from A. Birch (MPS), G. Barnes, A. Crouch, T. Felipe, KD Leka (NWRA) M. Rempel, Y. Fan (NCAR) 2 outline meeting the challenges of
Helioseismic and Magnetic Imager for Solar Dynamics Observatory
Helioseismic and Magnetic Imager for Solar Dynamics Observatory Concept Study Report Appendix A HMI Science Plan SU-HMI-S014 2 July 2003 Stanford University Hansen Experimental Physics Laboratory and Lockheed-Martin
Chapter 8 The Sun Our Star
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 8 The Sun
CONSTRAINTS ON THE APPLICABILITY OF AN INTERFACE DYNAMO TO THE SUN
The Astrophysical Journal, 631:647 652, 2005 September 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. CONSTRAINTS ON THE APPLICABILITY OF AN INTERFACE DYNAMO TO THE
What does helioseismology tell us about the Sun?
What does helioseismology tell us about the Sun? Jørgen Christensen-Dalsgaard Department of Physics and Astronomy, University of Aarhus & Danish AsteroSeismology Centre (DASC) Sir Arthur Stanley Eddington:
Astronomy 1 Fall Reminder: When/where does your observing session meet? [See from your TA.]
![Astronomy 1 Fall Reminder: When/where does your observing session meet? [See from your TA.]](/thumbs/90/103712995.jpg "Astronomy 1 Fall Reminder: When/where does your observing session meet? [See from your TA.]")
Astronomy 1 Fall 2016 Reminder: When/where does your observing session meet? [See email from your TA.] Lecture 9, October 25, 2016 Previously on Astro-1 What is the Moon made of? How did the Moon form?
Astronomy 310/510: Lecture 2: In stars, hydrostatic equilbrium means pressure out cancels gravity in.
Astronomy 310/510: Lecture 2: Newton s laws, his second law in particular: F = ma. If a = 0, then no net forces act. In stars, hydrostatic equilbrium means pressure out cancels gravity in. When pressure
Solar Cycle Prediction and Reconstruction. Dr. David H. Hathaway NASA/Ames Research Center
Solar Cycle Prediction and Reconstruction Dr. David H. Hathaway NASA/Ames Research Center Outline Solar cycle characteristics Producing the solar cycle the solar dynamo Polar magnetic fields producing
Outline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.
Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned. Next homework due Oct 24 th. I will not be here on Wednesday, but Paul Ricker will present the lecture! My Tuesday
Advanced Stellar Astrophysics
v Advanced Stellar Astrophysics William K. Rose University of Maryland College Park CAMBRIDGE UNIVERSITY PRESS Contents Preface xiii Star formation and stellar evolution: an overview 1 1 A short history
AGENDA. Time Event Location 17:30-19:00 Registration Muller Rear Lobby 17:30-19:00 Welcome Reception Cafe Azafran
AGENDA Sunday, October 13, 2013 Time Event Location 17:30-19:00 Registration Muller Rear Lobby 17:30-19:00 Welcome Reception Cafe Azafran Monday, October 14, 2013 08:00-09:00 Registration Muller Rear Lobby
Stanford Helioseismology Workshop 6-9 August Sébastien Couvidat & Paul Rajaguru HEPL, Stanford University
Stanford Helioseismology Workshop 6-9 August 2007 Ring-Like Structures in the Travel-Time maps of Sunspots Sébastien Couvidat & Paul Rajaguru HEPL, Stanford University Time-Distance Helioseismology Phase-speed
Towards Waveform Heliotomography: Observing Interactions of Helioseismic Waves with a Sunspot
Solar Physics DOI: 10.1007/ - - - - Towards Waveform Heliotomography: Observing Interactions of Helioseismic Waves with a Sunspot Junwei Zhao Alexander G. Kosovichev Stathis Ilonidis c Springer Abstract
Calibrating Core Overshooting in Low-Mass Stars with Kepler Data
Calibrating Core Overshooting in Low-Mass Stars with Kepler Data S. Deheuvels 1,2 1 Université de Toulouse; UPS-OMP; IRAP; Toulouse, France 2 CNRS; IRAP; 14, avenue Edouard Belin, F-31400 Toulouse, France
4+ YEARS OF SCIENTIFIC RESULTS WITH SDO/HMI
4+ YEARS OF SCIENTIFIC RESULTS WITH SDO/HMI Sebastien Couvidat and the HMI team Solar Metrology Symposium, October 2014 The HMI Instrument HMI Science Goals Evidence of Double-Cell Meridional Circulation
Oscillations of the Sun: insights and challenges for the future
Mem. S.A.It. Vol. 74, 564 c SAIt 2003 Memorie della Oscillations of the Sun: insights and challenges for the future M. P. Di Mauro 1 and L. Paternò 2 1 INAF-Osservatorio Astrofisico di Catania via S. Sofia
Astronomy Mini-Conference Logistics
Astronomy Mini-Conference Logistics Who: Y all Also sponsored by the Wyoming NASA Space Grant Consortium (they re providing some funds for food-like items) What: Presentation of Posters You will have some
The physics of red-giant oscillations
The physics of red-giant oscillations Marc-Antoine Dupret University of Liège, Belgium The impact of asteroseismology across stellar astrophysics Santa Barbara, 24-28 oct 2011 Plan of the presentation
Lecture 14: Solar Cycle. Observations of the Solar Cycle. Babcock-Leighton Model. Outline
Lecture 14: Solar Cycle Outline 1 Observations of the Solar Cycle 2 Babcock-Leighton Model Observations of the Solar Cycle Sunspot Number 11-year (average) cycle period as short as 8 years as long as 15
"Heinrich Schwabe's holistic detective agency
"Heinrich Schwabe's holistic detective agency, Ricky Egeland* High Altitude Observatory, NCAR 1. Sun alone is a complex system, emergence, total is > Σ of parts=> holistic 2. The Sun alone has provided
Astronomy 114. Lecture 13: Energy generation, magnetic fields. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 13: Energy generation, magnetic fields Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 13 05 Mar 2007 Read: Ch. 19 Astronomy 114 1/17 Announcements
The Sun s Magnetic Cycle: Current State of our Understanding
The Sun s Magnetic Cycle: Current State of our Understanding Dibyendu Nandi Outline: The need to understand solar variability The solar cycle: Observational characteristics MHD: Basic theoretical perspectives;
Solar Seismic Model and the Neutrino Fluxes
Solar Seismic Model and the Neutrino Fluxes K. M. Hiremath Indian Institute of Astrophysics Bangalore-560034, India H. Shibahashi and M. Takata University of Tokyo, Japan 4/19/2006 1 Plan of the talk Introduction
Solar surface rotation
Stellar rotation Solar surface rotation Solar nearsurface rotation Surface Doppler Schou et al. (1998; ApJ 505, 390) Rotational splitting Inferred solar internal rotation Near solidbody rotation of interior
Introduction to the Summer Institute 2009
Introduction to the Summer Institute 2009 Introduction to the research infrastructure University&FZK KIT KCETA Aim and Structure of the Summer Institute programme & modules excursions registration & technicalities
Guidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.
Guidepost The Sun is the source of light an warmth in our solar system, so it is a natural object to human curiosity. It is also the star most easily visible from Earth, and therefore the most studied.
The Physics of Fluids and Plasmas
The Physics of Fluids and Plasmas An Introduction for Astrophysicists ARNAB RAI CHOUDHURI CAMBRIDGE UNIVERSITY PRESS Preface Acknowledgements xiii xvii Introduction 1 1. 3 1.1 Fluids and plasmas in the
15th High Energy Astrophysics Division Meeting Naples, Florida Sunday, 3 April :00 pm Registration, 3:00 pm 7:00 pm, Royal Palms Foyer Speaker
Sunday, 3 April 2016 3:00 pm Registration, 3:00 pm 7:00 pm, Royal Palms Foyer Speaker Ready, 3:00 pm 7:00 pm, Royal Palms 5 (back of room) 7:00 pm Opening Reception, 7:00 pm 8:30 pm, Vista Ballroom Monday,
Tatranska Lomnica, Slovakia School and Workshop:
Tatranska Lomnica, Slovakia School and Workshop: The 2nd SOLARNET School "Ground- and space- based solar instruments" was held in Tatranska Lomnica (Slovakia), October 5-16, 2014 http://www.astro.sk/solarnet_2nd_school/solarnet
CONSTRAINING MIXING PROCESSES IN 16CYGA USING KEPLER DATA AND SEISMIC INVERSION TECHNIQUES. Gaël Buldgen Pr. Marc-Antoine Dupret Dr. Daniel R.
CONSTRAINING MIXING PROCESSES IN 16CYGA USING KEPLER DATA AND SEISMIC INVERSION TECHNIQUES Gaël Buldgen Pr. Marc-Antoine Dupret Dr. Daniel R. Reese University of Liège June 215 GENERAL STRUCTURE OF THE
Astronomy Chapter 12 Review
Astronomy Chapter 12 Review Approximately how massive is the Sun as compared to the Earth? A. 100 times B. 300 times C. 3000 times D. 300,000 times E. One million times Approximately how massive is the
Ages of the oldest stars and the connection to the halo and accretion. Three questions about the ages of old stars
ages 2 : Taking stellar ages to the next power Daily Agenda Monday, September 18, 2017 Ages of the oldest stars and the connection to the halo and accretion 9:15 S. Cassisi, S. Degl Innocenti Three questions
The Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun
The Sun The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x 10 33 g = 330,000 M Earth = 1 M Sun Radius of Sun = 7 x 10 5 km = 109 R Earth = 1 R Sun Luminosity of Sun =
IPCC Workshop on Sea Level Rise and Ice Sheet Instabilities
IPCC Workshop on Sea Level Rise and Ice Sheet Instabilities Hilton Hotel, Kuala Lumpur, Malaysia 21-24 June 2010 PROGRAMME Sunday, 20 June 2010 18:00 19:30 Early Registration and Welcome Reception (Sponsored
The Origin of the Solar Cycle & Helioseismology
The Origin of the Solar Cycle & Helioseismology What is the solar cycle? Simple concept of cycle mechanism, dynamo What is helioseismology? Global properties of the solar interior Local properties of the
Correction to Homework
Today: Chapter 10 Reading Next Week: Homework Due March 12 Midterm Exam: March 19 Correction to Homework #1: Diameter of eye: 2.5 cm #10: See Ch. 11 Office Hours Monday. 11AM -2 PM Help Sessions Available:
Kwasan and Hida Observtories, Kyoto University 2
Journal of Integrated Creative Studies A Report on the Workshop Superflares on Solar-type Stars and Solar Flares, and Their Impacts on Exoplanets and the Earth. held in 2016 March 1st (Tue) March 4th (Fri)
The Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:
The Sun Basic Properties Radius: Mass: 5 R Sun = 6.96 km 9 R M Sun 5 30 = 1.99 kg 3.33 M ρ Sun = 1.41g cm 3 Luminosity: L Sun = 3.86 26 W Effective Temperature: L Sun 2 4 = 4πRSunσTe Te 5770 K The Sun
ASTR 100. Lecture 15: The Sun
ASTR 100 Lecture 15: The Sun Start reading about: The Sun (Ch. 10), Spectra (Ch. 5), Stars (Ch. 11) Next week: Stars and Spectra Midterm: Tuesday, February 18 th UW planetarium: Tuesday, March 4 th 3:00pm
Obridko V., Georgieva K. June 6-10, 2016, Bulgaria
First VarSITI General Symposium Solar activity in the following decades based on the results of the ISSI/VarSITI Forum on future evolution of solar activity, 01.03-03.03.2015 ISSI, Bern, Switzerland Obridko
The Future of Helio- and Asteroseismology (L.Gizon)
The Future of Helio- and Asteroseismology (L.Gizon) Millions of modes of vibration, excited by turbulent convection, permeate the solar interior. Surface observations of the motions caused by these waves
BepiColombo SWT # October 2017, Matera
BepiColombo SWT #16 23 27 October 2017, Matera Hotel San Domenico al Piano Via Roma 15 - Matera (Italy) 23 October 2017 9:15 Participant welcome 9:30 BepiColombo HEWG splinter agenda see below 18:00 End
arxiv: v1 [astro-ph] 2 Oct 2007
![arxiv: v1 [astro-ph] 2 Oct 2007](/thumbs/94/121336069.jpg "arxiv: v1 [astro-ph] 2 Oct 2007")
Speed of Meridional Flows and Magnetic Flux Transport on the Sun Michal Švanda, 1,2, Alexander G. Kosovichev 3, and Junwei Zhao 3 arxiv:0710.0590v1 [astro-ph] 2 Oct 2007 ABSTRACT We use the magnetic butterfly
Helioseismic and Magnetic Imager for Solar Dynamics Observatory
for Solar Dynamics Observatory HMI Science Plan Including Science Requirements SU-HMI-S014 CDR Version - 9 November 2004 Stanford University Hansen Experimental Physics Laboratory and Lockheed-Martin Solar
Supplementary Figure 1 Comparison of the distribution of S indices measured by LAMOST (red) and the distribution measured by Isaacson & Fischer 57
Supplementary Figure 1 Comparison of the distribution of S indices measured by LAMOST (red) and the distribution measured by Isaacson & Fischer 57 (black). Isaacson and Fischer observe more high-activity
2. Stellar atmospheres: Structure
2. Stellar atmospheres: Structure 2.1. Assumptions Plane-parallel geometry Hydrostatic equilibrium, i.e. o no large-scale accelerations comparable to surface gravity o no dynamically significant mass loss
Reconstructing the Subsurface Three-Dimensional Magnetic Structure of Solar Active Regions Using SDO/HMI Observations
Reconstructing the Subsurface Three-Dimensional Magnetic Structure of Solar Active Regions Using SDO/HMI Observations Georgios Chintzoglou*, Jie Zhang School of Physics, Astronomy and Computational Sciences,
McMath-Pierce Adaptive Optics Overview. Christoph Keller National Solar Observatory, Tucson
McMath-Pierce Adaptive Optics Overview Christoph Keller National Solar Observatory, Tucson Small-Scale Structures on the Sun 1 arcsec Important astrophysical scales (pressure scale height in photosphere,
The Sun as Our Star. Properties of the Sun. Solar Composition. Last class we talked about how the Sun compares to other stars in the sky
The Sun as Our Star Last class we talked about how the Sun compares to other stars in the sky Today's lecture will concentrate on the different layers of the Sun's interior and its atmosphere We will also
Astr 1050 Mon. March 30, 2015 This week s Topics
Astr 1050 Mon. March 30, 2015 This week s Topics Chapter 14: The Sun, Our Star Structure of the Sun Physical Properties & Stability Photosphere Opacity Spectral Line Formation Temperature Profile The Chromosphere
Diffusion and helioseismology
Diffusion and helioseismology Jørgen Christensen-Dalsgaard Institut for Fysik og Astronomi, Aarhus Universitet & Danish AsteroSeismology Centre (DASC) Eddington (1926): The internal constitution of the
Interpreting HMI multi-height velocity measurements Kaori Nagashima
Interpreting HMI multi-height velocity measurements Kaori Nagashima Postdoc of Interior of the Sun and Stars Dept. @MPS (May 2012 - ) Collaborators of this study: L. Gizon, A. Birch, B. Löptien, S. Danilovic,
INFERENCE OF SOLAR SUBSURFACE FLOWS BY TIME-DISTANCE HELIOSEISMOLOGY
INFERENCE OF SOLAR SUBSURFACE FLOWS BY TIME-DISTANCE HELIOSEISMOLOGY a dissertation submitted to the department of physics and the committee on graduate studies of stanford university in partial fulfillment
Stellar noise: physics and mechanisms
Stellar noise: physics and mechanisms Ignasi Ribas Institut de Ciències de l Espai (CSIC IEEC, Barcelona) Leiden, October 2012 Stellar signal: physics and mechanisms Ignasi Ribas Institut de Ciències de
Program. 09:00 09:45 Tilman Esslinger A cold grip on topology: the Haldane model
Sunday, 8 May 2016 17:00 21:00 Registration 18:00 DINNER / Informal get together Monday, 9 May 2016 08:50 09:00 Axel Pelster Opening and Welcome Session 1: Topology 09:00 09:45 Tilman Esslinger A cold
Ulugh Beg Astronomical Institute of Uzbek Academy of Sciences history and current status of solar physics research
First Asia-Pacific Solar Physics Meeting ASI Conference Series, 2011, Vol. 2, pp 405 409 Edited by Arnab Rai Choudhuri & Dipankar Banerjee Ulugh Beg Astronomical Institute of Uzbek Academy of Sciences
Announcements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11
Announcements - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Review for Test #2 Oct 11 Topics: The Solar System and its Formation The Earth and our Moon
Framework programme of 5th International Olympiad on Astronomy and Astrophysics
Framework programme of 5th International Olympiad on Astronomy and Astrophysics Day 1 25th August 2011 Thursday & Arrival to Poland transfer from the airport\train station to the appropriate hotel. The
Chapter 14 Lecture. Chapter 14: Our Star Pearson Education, Inc.
Chapter 14 Lecture Chapter 14: Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on FIRE?
Ay 1 Lecture 8. Stellar Structure and the Sun
Ay 1 Lecture 8 Stellar Structure and the Sun 8.1 Stellar Structure Basics How Stars Work Hydrostatic Equilibrium: gas and radiation pressure balance the gravity Thermal Equilibrium: Energy generated =
Seminar: Measurement of Stellar Parameters with Asteroseismology
Seminar: Measurement of Stellar Parameters with Asteroseismology Author: Gal Kranjc Kušlan Mentor: dr. Andrej Prša Ljubljana, December 2017 Abstract In this seminar I introduce asteroseismology, which
Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Observing Highlights. Stars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Announcements Lab Observing Trip Next week: Tues (9/28) & Thurs (9/30) let me know ASAP if you have an official conflict (class, work) - website: http://astro.physics.uiowa.edu/~clang/sgu_fall10/observing_trip.html
Astronomy 404 October 18, 2013
Astronomy 404 October 18, 2013 Parker Wind Model Assumes an isothermal corona, simplified HSE Why does this model fail? Dynamic mass flow of particles from the corona, the system is not closed Re-write
arxiv: v1 [astro-ph.sr] 3 Nov 2010
![arxiv: v1 [astro-ph.sr] 3 Nov 2010](/thumbs/92/109675299.jpg "arxiv: v1 [astro-ph.sr] 3 Nov 2010")
arxiv:1011.0799v1 [astro-ph.sr] 3 Nov 2010 Local helioseismology of sunspot regions: comparison of ring-diagram and time-distance results A.G. Kosovichev 1, S. Basu 2, R. Bogart 1, T.L. Duvall, Jr 3, I.
UNIT 3: Astronomy Chapter 26: Stars and Galaxies (pages )
CORNELL NOTES Directions: You must create a minimum of 5 questions in this column per page (average). Use these to study your notes and prepare for tests and quizzes. Notes will be turned in to your teacher
Chapter 14 Our Star A Closer Look at the Sun. Why was the Sun s energy source a major mystery?
Chapter 14 Our Star 14.1 A Closer Look at the Sun Our goals for learning Why was the Sun s energy source a major mystery? Why does the Sun shine? What is the Sun s structure? Why was the Sun s energy source
Asteroseismology of red giants. M Vrard, Elbereth, 25 november
Asteroseismology of red giants M Vrard, Elbereth, 25 november 2013 1 Introduction : what is a red giant? -These stars have finished to burn their hydrogene in their core -They progress through various
Asteroseismology of Red Giants. Josefina Montalbán Université de Liège
Asteroseismology of Red Giants Josefina Montalbán Université de Liège Stellar oscillations Oscillation mode Variations of v r : spectroscopy Variations of luminosity: photometry Basic properties Lamb Frequency:
Types of Stars 1/31/14 O B A F G K M. 8-6 Luminosity. 8-7 Stellar Temperatures
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars For nearby stars - measure distances with parallax 1 AU d p 8-2 Parallax A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3
Lecture 1: Introduction. Literature: Onno Pols chapter 1, Prialnik chapter 1
Lecture 1: Introduction Literature: Onno Pols chapter 1, Prialnik chapter 1!" Goals of the Course! Understand the global characteristics of stars! Relate relevant microphysics to the global stellar characteristics!