Paul Bryans

Chasing the IR Corona through Solar Eclipse Experiments

whawkins — Tue, 16 Apr 2024 19:21:26 +0000

Chasing the IR Corona through Solar Eclipse Experiments whawkins Tue, 04/16/2024 - 13:21

Author:

whawkins

Apr 16, 2024

Composite image of the eclipse as seen from Dardanelle, AR. A narrow H-alpha filter was used to capture the emission of the solar disk during the partial phases of the eclipse, while the totality phase was captured in white light emission.

The total solar eclipse on April 8, 2024, was a great opportunity for the team of HAO, NSO, and NOAA scientists and collaborators to travel to a location on the totality path with the goal of running unique science experiments. Using additional telescopes, binoculars, and outreach materials, we were able to capture the eclipse throughout its phases and share our passion with a very excited local crowd.

Two eclipse science experimental setups were designed and built by our team at the HAO facility and tuned to observe the infrared solar corona during the totality phase of the eclipse: the Coronal HElium Emission Spectrograph Experiment (CHEESE) led by HAO’s Momchil Molnar and FeSun (read Iron Sun) led by NSO's Alin Paraschiv. CHEESE is a high-resolution spectrograph and FeSun is a coronagraphic filter imager designed to build a mosaic of the corona. We hope to reveal new and exciting science using emission lines of Iron and Helium that form in the infrared range of the light spectrum.

The two eclipse experiments are assembled and waiting for final adjustments.

The eclipse team consisted of Momchil Molnar, Alin Paraschiv (NSO), Maurice Wilson, David Afonso Delgado, Gabriel Dima (NOAA), Daniela Lacatus, Paul Bryans, and Kalista Tyson (student). The whole expedition was a huge adventure for our team, and after some rollercoaster moments, we successfully achieved perfect weather conditions through the entire eclipse; considering what we went through, this was no small feat! (Now that the expedition is over we begin the long task of analyzing and interpreting our infrared science data to uncover new coronal insights.)

Fredericksburg, TX, was our initial and carefully chosen location. Unfortunately, after a 10-hour drive there, we understood our eclipse viewing chances were extremely slim due to overcast skies. Suddenly we were scrambling to find a better location; we decided to drive northeast another 10 hours to Dardanelle, AR. The extra day of driving was a hardship and we missed a night of testing. Sadly, we left Paul behind because he was meeting his family in Texas. Happily, our change of location to Arkansas was a great success as the weather was lovely, with clear skies throughout the eclipse!

On Sunday morning, before the Monday eclipse, Alin and Momo (experiment leads) finally started assembling the experiments. In utter horror they realized that we were missing one of four boxes containing the crucial mount heads for both experiments. This became a joke of how many PhDs does it take to account for four boxes and load those boxes into cars.

Luckily, Kalista Tyson (former REU student and HAO visitor), came to our rescue with a special delivery, arriving at our location in Arkansas on Monday at 4am, with the "invisible at departure box." With sleep deprived eyes, we rushed to assemble the experiments and do as much of the alignment and testing in a few hours, instead of the planned preparation time of two days and two nights. In addition, we had to address some issues that were not completely ironed out, especially given the change in location. Despite it all, the experiments executed their observation sequences, and data was acquired.

The experiments PIs doing final adjustments to the instruments as the eclipse approaches the totality phase. (P.S. ‘Bene Gesserit’ infiltrators were on site if you look carefully!)

We also had a telescope dedicated to capturing the solar disk in H-alpha emission throughout the eclipse phases. The composite image above illustrates the capture results beautifully. An additional telescope plus two pairs of binoculars were available to provide the public with a closer view of the eclipse progression and enabled them to photograph the solar disk being gradually obscured.

In addition to the science experiments, we also had a telescope and binoculars available for the public, as well as a booth where we shared cool science tidbits and answered questions.

At the outreach booth we provided materials on eclipses, the sun, its structure and phenomena, plus its influence on the solar system. We also introduced the pinhole concept for safe eclipse viewing. The public was excited to have “real scientists doing science” in a backyard, small-town setting where they were comfortable interacting and asking questions. We were energized by their science queries and curiosities about the broader impact of our work and science in general.

Moments before totality, everyone was getting ready to enjoy the astronomical show and/or watch the excitable scientists acquire their data.

Once the eclipse ended, we rushed to pack up everything because a storm front was arriving with intense rain and winds. While some of us began driving back that evening, other team members stayed another night. Due to heavy rains, they became stuck in the mud and had to be pulled out by a tractor the following morning. The first group arrived back to Boulder on Tuesday near midnight, while the campervan group arrived after 4am on Wednesday morning.

The enormous effort that went into preparing the experiments and the actual expedition was definitely worth it. We learned a lot by building and deploying the experiments in the eclipse path, and in spite of some setbacks, both experiments ran successfully and data was acquired! In addition, we got to experience a unique astronomical event, share our passion for science and solar physics in particular, and hopefully make a lasting impression on our public audience.

We want to emphasize once again our immense gratitude to Kalista for dropping everything without a second thought and driving to our rescue! Without her swift intervention, all the effort invested in preparing the experiments would have been futile!

Furthermore, we are grateful to Skylar Shaver and the Ring family for graciously hosting us on their property in Dardanelle, Arkansas, on very short notice. Because of their generosity and in spite of the impromptu change in location, we were able to set up our experiments and our outreach booth. Best of all, we ended the day sharing the total eclipse experience with ~80 people and 8 dogs.

We want to thank everyone who made this expedition possible: members, mentors, institutions, friends and family! We are grateful to Paul Bryans and Sheryl Shapiro for their work on coordinating the logistics and making sure this adventure could happen (plus Paul’s sacrifice during the trip). We are also grateful to Roberto Casini, Matthias Rempel, Ben Berkey, Alfred de Wijn, Phil Judge, Kevin Reardon (NSO), and Tom Schad (NSO) for their guidance, support and insights on how to run eclipse experiments, things to consider, and for giving us a hand when we inadvertently got stuck. And last but not least, we want to thank Holly Gilbert for ensuring this effort had adequate resources, without which nothing would have been possible.

Story by Daniela Lacatus, edited by Wendy Hawkins

WHPI repository of 2024 Total Solar Eclipse activities

whawkins — Tue, 19 Mar 2024 16:14:43 +0000

WHPI repository of 2024 Total Solar Eclipse activities whawkins Tue, 03/19/2024 - 10:14

Author:

whawkins

Mar 19, 2024

HAO is leading the effort through the Whole Heliosphere and Planetary Interactions (WHPI) initiative to support the 2024 Total Solar Eclipse by providing a platform for gathering information on ongoing eclipse activities. The WHPI Eclipse Campaign website aims to be a one-stop repository for existing or ongoing eclipse efforts.

The Total Solar Eclipse on April 8, 2024 offers ideal conditions for eclipse science, unique opportunities for cross-disciplinary collaborations, and an excellent occasion for public engagement. HAO is leading the effort through the Whole Heliosphere and Planetary Interactions (WHPI) initiative to support the 2024 Total Solar Eclipse by providing a platform for gathering information on ongoing eclipse activities. The WHPI Eclipse Campaign website aims to be a one-stop repository for existing or ongoing eclipse efforts. We welcome any and all contributions, no effort is too small! Please contact us at whpi_help@hao.ucar.edu if you have any questions or would like to be included.

The repository is currently:

Linking to model prediction outputs of what to expect on the eclipse day;
Providing information on planned dedicated observations by ground and space-based assets that will pursue and support eclipse science;
Compiling a list of eclipse science experiments that will be deployed on or flown into the eclipse path;
Providing information on Citizen Science projects those interested can join in;
Listing planned outreach and public engagement efforts.

We hope our repository will promote interactions between the different efforts and foster collaboration across disciplines. We wish everyone a clear sky and happy observing of the eclipse!

International UCoMP Users Workshop

whawkins — Thu, 07 Sep 2023 19:23:33 +0000

International UCoMP Users Workshop whawkins Thu, 09/07/2023 - 13:23

Author:

whawkins

Sep 7, 2023

Steve displaying slides at UCoMP users workshop.

HAO director Holly Gilbert comments: "There was great energy around the UCoMP Users Workshop last week, with many visitors coming from around the world to participate. Thanks to those who made it a success, including many early career folks!"

The first-ever UCoMP Data User’s Workshop was held the week of August 29 and was a great success. The purpose was to introduce UCoMP to the community and to organize working groups to collaborate on UCoMP first results to be published in a topical issue of Solar Physics. The workshop combined tutorial-type presentations from the UCoMP team, discussions between the UCoMP team and users, user presentations, and hands-on activities for attendees. There were 41 attendees: 23 in-person and 18 remote. Recordings of the presentations can be found on the UCoMP Youtube channel.

Optimal spectral lines for measuring chromospheric magnetic fields

kolinski — Mon, 11 Jul 2022 20:33:01 +0000

Optimal spectral lines for measuring chromospheric magnetic fields kolinski Mon, 07/11/2022 - 14:33

Paul Bryans interviewed by Sun Superheroes

kolinski — Mon, 20 Dec 2021 19:16:54 +0000

Paul Bryans interviewed by Sun Superheroes kolinski Mon, 12/20/2021 - 12:16

Author:

kolinski

Dec 20, 2021

Solar Eclipse Team, Chile, 2019.

Paul Bryans tells Sun Superheroes that a solar eclipse is an opportunity to understand and study the Sun's magnetism. During a solar eclipse, when the moon blocks the Sun, it allows scientists to study the strength and shape of the Sun's surrounding magnetic field. The Sun's energy is completely magnetic and the more we understand its magnetism, the better we can predict coronal mass ejections, flares, and other explosive events that can impact the Earth's electric grid.

Paul explains that as a child he had no plans to become a Sun scientist. In highschool he enjoyed math and science and while studying physics in college he was offered a summer internship at a government Solar Physics lab in England. That experience sparked his interest and he has been studying the Sun ever since. Paul encourages everyone to make an effort to personally witness a total eclipse at least once in their lifetime. Experiencing a total eclipse is special, Paul says, when your surroundings become dark, then cold, and the stars appear in the middle of the day. The next total eclipse in the United States will be in 2024.

Sun SuperHeroes interviewed Dr. Paul Bryans of the High Altitude Observatory about his recent excursion to the Cerro Tololo Inter American Observatory in Chile to observe a total solar eclipse.

BACSMediaLab

AAS Nova Features a Recent Publication by Philip Judge

kolinski — Thu, 18 Nov 2021 19:36:28 +0000

AAS Nova Features a Recent Publication by Philip Judge kolinski Thu, 11/18/2021 - 12:36

Author:

kolinski

Nov 18, 2021

Understanding the magnitude and occurrence of solar storms is key to predicting events that can be harmful to thousands of Earth-orbiting satellites and the welfare of astronauts. A recent paper by Philip Judge et al was highlighted in AAS Nova in a their featured article entitled, "A Better Space Weather Forecasting Tool."

Images to highlight the corrugated surfaces at which the centers of UV lines are formed (close to τ = 1) in MURaM calculations of the upper solar chromosphere. The calculations are from a numerical experiment where a magnetic flux system is emerging from beneath the solar atmosphere. The emergent fields carry with them plasma, which is revealed by the extended heights of the τ = 1 surfaces, which can exceed 10 Mm. Typically the Doppler line shifts in the lower transition region are smaller than the line widths (Athay & Dere 1991). Therefore the τ = 1 surfaces were computed without taking into account Doppler shifts, at the centers of lines of Mg ii k, and several lines of Fe ii. The x–y images of height of formation are plotted in order of decreasing opacity from Mg ii to Fe ii 2769.75 Å. In the bottom right panel, slices of these τ = 1 surfaces are shown, taken along the black line in the five other panels. But the black lines in this final panel are magnetic lines of force in the y–z plane. Evidently, a combination of these and other lines of iron with a wide range of opacities spans the ranges of excursions of the surfaces away from a horizontal plane.

Link to paper: Measuring the Magnetic Origins of Solar Flares, Coronal Mass Ejections, and Space Weather

A new facility for airborne solar astronomy: NASA’s WB-57 at the 2017 total solar eclipse

kolinski — Thu, 18 Nov 2021 17:11:37 +0000

A new facility for airborne solar astronomy: NASA’s WB-57 at the 2017 total solar eclipse kolinski Thu, 11/18/2021 - 10:11

Publication Name: ApJ; First HAO Author's Name: Paul Bryans; Authors names as they are listed in article: Amir Caspi, Daniel B. Seaton, Constantine C. C. Tsang, Craig E. DeForest, Paul Bryans, Edward E. DeLuca, et al.

Author:

kolinski

Nov 18, 2021

NASA's WB-57 High Altitude Research Program provides a deployable, mobile, stratospheric platform for scientic research. Airborne platforms are of particular value for making coronal observations during total solar eclipses because of their ability both to follow the Moon's shadow and to get above most of the atmospheric airmass that can interfere with astronomical observations.

Fully processed image of the corona generated by stacking many co-aligned, calibrated images and applying a radial filter and multi-scale unsharp mask to bring out details at higher altitudes.

We used the 2017 Aug 21 eclipse as a pathfinding mission for high-altitude airborne solar astronomy, using the existing high speed visible-light and near-/mid-wave infrared imaging suite mounted in the WB-57 nose cone. In this paper, we describe the aircraft, the instrument, and the 2017 mission; operations and data acquisition; and preliminary analysis of data quality from the existing instrument suite. We describe benets and technical limitations of this platform for solar and other astronomical observations. We present a preliminary analysis of the visible-light data quality and discuss the limiting factors that must be overcome with future instrumentation. We conclude with a discussion of lessons learned from this pathnding mission and prospects for future research at upcoming eclipses, as well as an evaluation of the capabilities of the WB-57 platform for future solar astronomy and general astronomical observation.

Detecting the Chromospheric Footpoints of the Solar Wind

kolinski — Tue, 16 Nov 2021 21:53:48 +0000

Detecting the Chromospheric Footpoints of the Solar Wind kolinski Tue, 11/16/2021 - 14:53

Publication: ApJL; Authors: Paul Bryans, Scott McIntosh, David Brooks, Bart De Pontieu

Author:

kolinski

Nov 16, 2021

Coronal Holes present the source of the fast solar wind. However, the fast solar wind is not unimodal—there are discrete, but subtle, compositional, velocity, and density structures that differentiate different coronal holes as well as wind streams that originate within one coronal hole. In this Letter we exploit full-disk observational “mosaics” performed by the Interface Region Imaging Spectrograph (IRIS) spacecraft to demonstrate that significant spectral contrast exists within the chromospheric plasma of coronal holes.

SDO and IRIS full-disk observations from 2016 Feb 22. The HMI and AIA Frankenmaps (panels A and B) are constructed of sub-images with the same fields of view and timing of the IRIS rasters that comprise the mosaic. The CHs in the northern hemisphere and at the south pole are most evident in the AIA intensity image (B), but not in Mg II intensity (C). The CHs are evident, however, in the Mg II peak separation map (D). After removing the center-to-limb variation, this is even clearer (F).

The spectral contrast seen delineates topological differences within the globally open structure. In particular, we show that the “peak separation” of the Mg II h line at 2803 A illustrates changes in what appear to be open magnetic features within a coronal hole. These observations point to a chromospheric source for the inhomogeneities found in the fast solar wind. These chromospheric signatures can provide additional constraints on magnetic field extrapolations close to the source, potentially on spatial scales smaller than from traditional coronal hole detection methods based on intensity thresholding in the corona. This is of increased importance with the advent of Parker Solar Probe and Solar Orbiter and the ability to accurately establish the connectivity between their in situ measurements and remote sensing observations of the solar atmosphere.

Paul Bryans

Chasing the IR Corona through Solar Eclipse Experiments

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