A Long-term Sunspot Magnetic Field Decrease

Slides:

Advertisements

Similar presentations

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

Advertisements

Microwave fluxes in the recent solar minimum H. Hudson, L. Svalgaard, K. Shibasaki, K. Tapping The time series of solar microwave flux traditionally is.

The Sun – Describe characteristics of the Sun (S6C3PO2 high school)

4/18 6:08 UT 4/17 6:09 UT Average polar cap flux North cap South cap… South cap South enter (need to modify search so we are here) South exit SAA Kress,

Sixty+ Years of Solar Microwave Flux Leif Svalgaard Stanford University SHINE 2010, Santa Fe, NM.

Long-term evolution of magnetic fields on the Sun Alexei A. Pevtsov US National Solar Observatory.

High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.

THE SUN: AWESOME AND ACTIVE

Measuring the Wilson effect: observations and modeling with RHESSI H. Jabran Zahid M. D. Fivian H. S. Hudson.

The Change of Magnetic Inclination Angles Associated with Flares Yixuan Li April 1,2008.

The Sun- Our Star. The Sun- Our Star Star Parts: core radiation zone convection zone photosphere chromosphere corona solar wind.

What stellar properties can be learnt from planetary transits Adriana Válio Roque da Silva CRAAM/Mackenzie.

Solar Rotation Lab 3. Differential Rotation The sun lacks a fixed rotation rate Since it is composed of a gaseous plasma, the rate of rotation is fastest.

An Introduction to Helioseismology (Local) 2008 Solar Physics Summer School June 16-20, Sacramento Peak Observatory, Sunspot, NM.

EARTH & SPACE SCIENCE Chapter 29 The Sun 29.2 Solar Activity.

The Sun Earth Science - Mr. Gallagher. The Sun is the Earth's nearest star. Similar to most typical stars, it is a large ball of hot electrically charged.

AOS 101 Weather and Climate Lisha M. Roubert University of Wisconsin-Madison Department of Atmospheric & Oceanic Sciences.

Energy Transport and Structure of the Solar Convection Zone James Armstrong University of Hawai’i Manoa 5/25/2004 Ph.D. Oral Examination.

The Sun & Stars, Galaxies, & the Universe. Composition & Age of the Sun Hydrogen and helium make up over 99% of the sun’s mass. About 75% of the sun’s.

Solar Cycle 24 Carl Luetzelschwab K9LA QCWA Chap 36 April 2012 K9LA.

Facts about the sun Sun Cycle Layers of the sun Sun’s Energy Terms Magnetic field $ 200 $ 200$200 $ 200 $ 200 $400 $ 400$400 $ 400$400 $600 $ 600$600.

Multi-level observations of magneto- acoustic cut-off frequency Ding Yuan Department of Physics University of Warwick Coventry CV4 7AL, UK

The Sun- Solar Activity. Damage to communications & power systems.

1 The Spots That Won’t Form Leif Svalgaard Stanford University 3 rd SSN Workshop, Tucson, AZ, Jan

Ch. 26.1: Our Sun!.

Solar Maximum ! A Double Peaked Sunspot Cycle ?

The Rise of Solar Cycle 24: Magnetic Fields from the Dynamo through the Photosphere and Corona and Connecting to the Heliosphere Part 1: Interior and Photosphere.

Fractal Dimension and Maximum Sunspot Number in Solar Cycle R.-S. Kim 1,2, Y. Yi 1, S.-W. Kim 2, K.-S. Cho 2, Y.-J. Moon 2 1 Chungnam national University.

PHYS 1621 Proton-proton cycle 3 steps. PHYS 1622 Layers of the Sun Mostly Hydrogen with about 25% Helium. Small amounts of heavier elements Gas described.

The Sun Youra Taroyan. Age 4.5 ×10 9 years Mean diameter 1.392×10 6 km, 109 × Earth Mass ×10 30 kg, 333,000 × Earth Volume 1.412×10 18 km 3, 1,300,000.

The Magnetic Sun. What is the Sun? The Sun is a Star, but seen close-up. The Stars are other Suns but very far away.

Reconstruction of solar irradiance variations in cycles 21, 22 and 23 based on surface magnetic fields Thomas Wenzler Institute of Astronomy ETH Zurich.

The Sun Composed of hydrogen and helium. Very dense core, all gaseous because of the very high temperatures. The Sun is the largest object in terms of.

Units to cover: 52, 53, Observatories in Space.

1 Grades 6-8: Introduction. 2 Aerospace Technology Space Science Human Exploration And Development Of Space Earth Science Main Areas Of Research.

Sun Notes. Characteristics CLOSEST star to earth CLOSEST star to earth The bright star in the center is Proxima Centauri.

CSI /PHYS Solar Atmosphere Fall 2004 Lecture 04 Sep. 22, 2004 Solar Magnetic Field, Solar Cycle, and Solar Dynamo.

Robin, Paul, Laura.  16 kilometers to 160,000 kilometers in size  None to hundreds  1 to 100 days  Umbra (4500K)  Penumbra(5500K)  Photosphere(5800K)

Ch Solar Activity. Sunspots Gases inside the sun move up and down due to convection and the sun’s magnetic fields. Regions of the photosphere are.

Chapter 28 The Sun Section 2 Solar Activity Notes 28-2.

The Sun. What do you know about the Sun? Sun Facts The Sun is a normal G2 star, one of more than 100 billion stars in our galaxy. It is closer to Earth.

EARTH SUN (SOL) Radius = 1 Radius = 109 Density =1 Density = Gravity =1 Gravity = 28.0 Temperature ~ 300K Temperature ~ 5,800K.

Part 4: The Stars In Part 3 we looked at the Solar System, that is, we looked at all the parts except for the central element: the sun. In Part 4 we are.

© 2017 Pearson Education, Inc.

The Sun Essential Question: What are the properties of the Sun?

Size, Heat, and Structure

Surface Temperature and Blackbodies Surface temperature: the temperature of the visible disk of the Sun (photosphere) blackbody: a perfect radiator.

California Standards: 1a, e.

What is the most basic reaction that happens in the sun?

Magnetic Field.

What is the fate of our sun and other stars?

The Sun *Our closest star

Ch. 26.1: Our Sun!.

Prepare your scantron:

Section 2: Solar Activity

Rick Leske, A. C. Cummings, R. A. Mewaldt, and E. C. Stone

WHAT IS THE SUN? The Sun is the star centre of the solar system. It consists of hot plasma and magnetic fields. The sun consists of hydrogen and helium.

For a given CA II K-line index there are too few sunspots after 2000

Solar Activity Chapter 8 Section 3.

The Sun’s Layers and Solar Activity

Sunspots Sunspots are the most well known feature on the photosphere. They are a region of the solar surface that is dark and relatively cool; and has.

Grades 9-12: Introduction

The sun gives off tremendous amounts of energy

Boyle’s Law: Pressure and Volume

Measurements of lifetimes of high-l solar p-modes in sunspots

B. L. Alterman & Justin C. Kasper July 18, 2019

Presentation transcript:

A Long-term Sunspot Magnetic Field Decrease William Livingston (NSO) Rachel MacDonald (Yale) Tom Schad (UAz) 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Dark umbral cores observed Intro to spectra 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Magnetostatics can be used to describe horizontal pressure balance between spot and surrounding solar photosphere. 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Magnetostatics can be used to describe horizontal pressure balance between spot and surrounding solar photosphere. Pp = nkTp Ps = nkTs + magnetic pressure 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Jaeggli 2009 If sunspot magnetic fields changed, and the solar photosphere remained constant, then the sunspot temperatures should also change: this would impact the sunspot intensities, and the abundance of molecules. Solid: 18 Sep 98, I=.55 Iqs Dashed: 27 Dec 05, I=.78 Iqs 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop KPVT data archive First work: 4000 spots: Imin,Numbra Current work: 13,000 spots, Imin, Numbra, Magnetic Field 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Although variations in Intensity were seen, no radius change was seen in this sample from the archive. This was in conflict with well-known empirical B vs radius correlations. 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop The automated sampling also showed that the B vs. radius relationship remained constant through solar cycle 23. 30 Apr 2010 Space Weather Workshop

Space Weather Workshop The automated sampling also showed that the B vs. radius relationship remained constant through solar cycle 23. Only small changes were seen in I and B vs. time in the larger sample, but importantly the change seen were fully accounted for by changes in the radius 30 Apr 2010 Space Weather Workshop

Space Weather Workshop The automated sampling also showed that the B vs. radius relationship remained constant through solar cycle 23. Only small changes were seen in I and B vs. time in the larger sample, but importantly the change seen were fully accounted for by changes in the radius Conclusion: the fundamental structure of a sunspot doesn’t change through the cycle… the only support for the IR measurements is a slightly changing mean radius. 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Introduction 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Introduction 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Introduction 30 Apr 2010 Space Weather Workshop

Space Weather Workshop Introduction 30 Apr 2010 Space Weather Workshop

Conservative interpretation The distribution of the sunspot magnetic fields during the declining phase of the sunspot cycle are different from the fields during the rise phase of the sunspot cycle. 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

Space Weather Workshop 30 Apr 2010 Space Weather Workshop

…possible implication Making three assumptions: Livingston’s cycle 23 IR measurements represent the “true” sunspot magnetic field probability distribution function There is a real physical cut-off so that no sunspots form with maximum magnetic fields less than 1500G The decrease in the mean field continues …then Solar cycle 24 will peak with a spot number of 57, and cycle 25 will peak with a spot number of 3. 30 Apr 2010 Space Weather Workshop

Critical observations IR measurements of the true B field strength in sunspots must be made in the next sunspot cycle 30 Apr 2010 Space Weather Workshop

Critical observations IR measurements of the true B field strength in sunspots must be made in the next sunspot cycle Will umbrae with B>3000G return? 30 Apr 2010 Space Weather Workshop

Critical observations IR measurements of the true B field strength in sunspots must be made in the next sunspot cycle Will umbrae with B>3000G return? Will most cycle 24 spots have B<2000G? 30 Apr 2010 Space Weather Workshop

Critical observations IR measurements of the true B field strength in sunspots must be made in the next sunspot cycle Will umbrae with B>3000G return? Will most cycle 24 spots have B<2000G? Efforts are underway to cross-calibrate Livingston’s observations with 2-D maps of the IR sunspot magnetic fields from the NAC. 30 Apr 2010 Space Weather Workshop