Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO

Slides:

Advertisements

Similar presentations

What is the fate of our sun and other stars?

Advertisements

The Science of Solar B Transient phenomena – this aim covers the wide ranges of explosive phenomena observed on the Sun – from small scale flaring in the.

Source: HAO's PSPT project These images were taken by the Precision Solar Photometric Telescope at Mauna Loa Solar Observatory in Hawaii. They show how.

ASPIICS on PROBA-3 Association de Satellites Pour l’Imagerie et l’Interférométrie de la Couronne Solaire San Diego, SPIE August, 26 th 2007 Sébastien Vives,

Stars and Galaxies The Sun.

Astronomy at Evergreen, 2003 an update from Dr. E.J. Zita Wed.8 Jan at SPSCC, 8:00 pm for the Southwest Washington Astronomical.

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

This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.

The Sun’s Dynamic Atmosphere Lecture 15. Guiding Questions 1.What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere.

This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.

Chapter 29 Review Stars.

The Hunt for a Link : Quantitative Connections Between Magnetic Fields and EIT Coronal Wave/CME Properties Prepared by James R. Robertson J.R. In conjunction.

Alfvén Waves in the Solar Corona S. Tomczyk, S. Mclntosh, S. Keil, P. Judge, T. Schad, D. Seeley, J. Edmondson Science, Vol. 317, Sep., 2007.

Show 1 -- photosphere & sunspots SUN COURSE - SLIDE SHOW 3 Show 2 -- corona & solar cycle Today: SOHO.

Chapter 7 The Sun. Solar Prominence – photo by SOHO spacecraft from the Astronomy Picture of the Day site link.

Sound Waves from the Northern Lights Photo courtesy of Bjorn Jorgensen, 18 January 2005, near Tromsø, Norway

The Sun is not a static body, but very active.The Sun is not a static body, but very active. Solar activity can have dramatic effects on the EarthSolar.

Conversations with the Earth Tom Burbine

Is There Life Out There? Our Solar System (and beyond) Draw a picture of what you think life would look like on another planet, if it existed. Describe.

Solar Eclipses. Solar eclipses: the big picture This drawing shows how the Sun, moon and Earth line up during a solar eclipse. The shadow area where you.

Cloud Imagery and Motion Mark Anderson, Scott Cornelsen, and Tom Wilkerson Space Dynamics Laboratory Utah State University, Logan, UT

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

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

The Sun Michael J Passow. General Characteristics Our closest star Source of almost all our energy One of 100 billion in the Milky Way Galaxy “average’

The Sun and the Heliosphere: some basic concepts…

The Sun Chapter 29 Section 29.2 and Spaceweather.

Solar Weather and Tropical Cyclone Activity Abstract Worldwide tropical cyclone energy and frequency data was obtained from the Unisys Weather database.

Curtis Walker – UCAR/SOARS/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

Chapter 9 The Sun. 9.4 The Active Sun Sunspots: appear dark because slightly cooler than surroundings:

The Sun Photo from

This work was performed under the auspices of the Significant Opportunities in Atmospheric Research and Science Program. SOARS is managed by the University.

The Wavelet Packets Equalization Technique: Applications on LASCO Images M.Mierla, R. Schwenn, G. Stenborg.

Advanced Solar Theory (MT5810) OUTLINE 1.Observational properties of the Sun 2.MHD equations (revision) 3.Induction equation - solutions when R m >1 4.Magnetic.

SOLAR FLARES AND ERUPTIONS Lyndsay Fletcher University of Glasgow.

Coronal magnetic fields Thomas Wiegelmann, MPI for Solar-System Research, (Former: MPI für Aeronomie) Katlenburg-Lindau Why are coronal magnetic fields.

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

Solar weather consists of the Sun’s effects upon its planetary system and the solar activities it causes. Solar activities, such as flares and CMEs, form.

Sunspot Telescope Sunspots and surface granulation are the two main features. Telescope: Celestron NexStar 5 mounted on a Losmandy mount. Field of View.

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

What can we learn about coronal mass ejections through spectroscopic observations Hui Tian High Altitude Observatory, National Center for Atmospheric Research.

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

Curtis Walker – UCAR/SOARS Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO.

Coronal Image Processing The Accurate Depiction of Structure in Qualitative Images of the White Light Corona Huw Morgan, Shadia Habbal, Richard Woo.

The Sun Created by the Lunar and Planetary Institute For Educational Use Only LPI is not responsible for the ways in which this powerpoint may be used.

Outer Layers of the Sun Photosphere –Limb darkening –Sun spots Chromosphere Corona Prominences, flares, coronal mass ejections Reading

Towards unambiguous characterization of coronal structures

Tracking Waves from Sunspots Provides New Solar Insight Zhau, J et. al

The Sun is “hot” Solar Eclipse Workshop May 20, 2017

On the three-dimensional configuration of coronal mass ejections

Solar Eclipses Solar Eclipses.

Scientists demonstrate a new Solar Energetic Particle warning technique using K-COR ground coronagraph data A Heliophysics science publication using ESA/NASA.

Coronal Magnetic Fields What are we learning from CoMP observations

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO

SLIDE SHOW 6. SOLAR WIND (Mariner 2, 1962)

Solar Eclipses Solar Eclipses.

Section 1: The Sun The Sun contains most of the mass of the solar system and has many features typical of other stars. K What I Know W What I Want to.

The Not-So-Calm After the Storm:

What is the fate of our sun and other stars?

Chromosphere Filters Kathy Geise.

Eclipse 2017 Offers Unique Opportunity for Science Investigations

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO

TABLE OF CONTENTS TABLE OF CONTENTS: Mission Overview Timeline

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO

Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO

The Centre of the Solar System Earth Science 11

The Comet Project: Image Processing s/k Keith Hawkins Sheena Patel.

Grades 9-12: Introduction

Astronomy notes for Phys/Geog 182

Solar Activity Forecast for the Next Decade

CORONAL MASS EJECTIONS

Presentation transcript:

Image Processing Algorithms for Aerosol Removal in Solar Coronal Images Curtis Walker – UCAR/SUNY Oneonta Scott Sewell – NCAR/HAO Steve Tomczyk – NCAR/HAO

Solar Corona Sun’s “Atmosphere” ~10⁶ K plasma Origin of the Solar Wind Emits massive quantities of energy Can only be seen during total solar eclipse Total solar eclipse, July 11, 1991, observed at Hawaii. Photo Credit: S. Koutcmy, IAP-CNRS (France)

Solar Coronagraph LASCO Satellite Photo Credit: NASA SOHO Instrumentation that produces a false eclipse of the sun allowing coronal observation Ground-based and satellite-based varieties Zeiss Coronagraph at Lomnicky Peak Observatory in Slovakia Photo Credit: Steve Tomczyk

Image Processing Dark Frame Corrections Flat Field Corrections Aerosol Removal

What Do Aerosols Look Like?

Measurement of Aerosol Motion The white tracks represent aerosol trajectories over ~1s. Final image processed of 120 images.

How Do We Correct For Aerosols? Three techniques for image thresholds Mean Threshold Median Threshold Minimum Threshold A series of 120 images containing atmospheric aerosols were obtained in Boulder, CO on June 16, 2010. The mean and median images were calculated.

Mean and Median Images Mean image of all 120 images. Note the aerosol streaks near the building and at left. Median image of all 120 images. Note that this is the best result.

Conclusions & Future Work We have obtained the necessary images (mean and median) to apply subsequent thresholding techniques. We will investigate optimizing these algorithms for real-time usage.