Maria D. Kazachenko
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View article: Signatures of Confined and Eruptive Solar Flares in Microwave Spectra
Signatures of Confined and Eruptive Solar Flares in Microwave Spectra Open
We describe how microwave spectra of confined flares differ from those of eruptive flares. All 29 confined ≥M1.4 soft X-ray flares from NOAA Active Region 12192 in 2014 October that were observed by the Radio Solar Telescope Network in the…
View article: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare Open
We detect rapid downflows of 150-217 km/s in IRIS Si IV 1402.77 nm measurements of an X9-class solar flare on 2024 October 3rd. The fast redshift values persist for over 15 minutes from flare onset, and can be split into two distinct stage…
View article: When Magnetic Field Lines Stretch, Snap, and Expand: A New Look at Solar Flares with L-maps
When Magnetic Field Lines Stretch, Snap, and Expand: A New Look at Solar Flares with L-maps Open
Understanding the three-dimensional evolution of coronal magnetic fields during solar flares remains challenging due to the lack of direct coronal field measurements. Here we combine data-driven MHD simulations of NOAA AR 11158 (Fan et al.…
View article: Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration
Genesis of a Confined X6.4 Flare in a Quadrupolar Magnetic Configuration Open
Both eruptive and confined flares—those having and lacking, respectively, an associated large-scale coronal mass ejection—are frequently observed in solar active regions (ARs). The physical mechanisms controlling the nature of these flares…
View article: Why every solar eclipse viewing event needs a disco ball
Why every solar eclipse viewing event needs a disco ball Open
Solar eclipses offer unparalleled opportunities for public engagement in astronomy. Large groups of people often gather to view eclipses, and these events require affordable and easy-to-use tools to safely observe the Sun. One unique way t…
View article: Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST
Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST Open
We present the highest-resolution H α observations of a solar flare to date, collected during the decay phase of an X1.3-class flare on 2024 August 8 at 20:12 UT. Observations with the Visible Broadband Imager at the National Science Found…
View article: Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST
Unveiling Unprecedented Fine Structure in Coronal Flare Loops with the DKIST Open
We present the highest-resolution H$α$ observations of a solar flare to date, collected during the decay phase of an X1.3-class flare on 8 August 2024 at 20:12 UT. Observations with the Visible Broadband Imager at the National Science Foun…
View article: Spectroscopic Observations of Supra-arcade Downflows
Spectroscopic Observations of Supra-arcade Downflows Open
Despite their somewhat frequent appearance in extreme-ultraviolet (EUV) imaging of off-limb flares, the origins of supra-arcade downflows (SADs) remain a mystery. Appearing as dark, tendril-like downflows above growing flare loop arcades, …
View article: Spectroscopic Observations of Supra-Arcade Downflows
Spectroscopic Observations of Supra-Arcade Downflows Open
Despite their somewhat-frequent appearance in EUV imaging of off-limb flares, the origins of Supra-Arcade Downflows (SADs) remain a mystery. Appearing as dark, tendril-like downflows above growing flare loop arcades, SADs themselves are ye…
View article: Spectral Irradiance Variability in Lyman-Alpha Emission During Solar Flares
Spectral Irradiance Variability in Lyman-Alpha Emission During Solar Flares Open
The Lyman-alpha (Ly $\alpha $ ; 1216 Å) line is the brightest emission line in the quiescent solar spectrum and radiates a significant fraction of the available nonthermal energy during flares. Despite its importance, there is a lack of …
View article: Spectral Irradiance Variability in Lyman-Alpha Emission During Solar Flares
Spectral Irradiance Variability in Lyman-Alpha Emission During Solar Flares Open
The Lyman-alpha (Lyα;1216 Å) line is the brightest emission line in the quiescent solar spectrum and radiates a significant fraction of the available nonthermal energy during flares. Despite its importance, there is a lack of detailed stud…
View article: Visible Eclipses through Clouds — a Challenge of Outreach Messaging
Visible Eclipses through Clouds — a Challenge of Outreach Messaging Open
View article: Eagle Pass, TX: The First American City on the Path of Totality: Organizing an Eclipse Party in the Stadium
Eagle Pass, TX: The First American City on the Path of Totality: Organizing an Eclipse Party in the Stadium Open
View article: X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
X-Ray and Spectral Ultraviolet Observations of Periodic Pulsations in a Solar Flare Fan/Looptop Open
We present simultaneous X-ray and spectral ultraviolet observations of strikingly coherent oscillations in emission from a coronal looptop and fan structure, during the impulsive phase of a long-duration M-class solar flare. The ≈50 s osci…
View article: Eagle Pass, TX: The First American City on the Path of Totality: Organizing Eclipse Party on the Stadium
Eagle Pass, TX: The First American City on the Path of Totality: Organizing Eclipse Party on the Stadium Open
In this paper we share the experience of the U.S. National Science Foundation (NSF) National Solar Observatory (NSO) scientists, educators and public outreach officers organizing an eclipse viewing party at a sports complex stadium on the …
View article: X-ray and Spectral UV Observations of Periodic Pulsations in a Solar Flare Fan/Looptop
X-ray and Spectral UV Observations of Periodic Pulsations in a Solar Flare Fan/Looptop Open
We present simultaneous X-ray and spectral ultraviolet (UV) observations of strikingly-coherent oscillations in emission from a coronal looptop and fan structure, during the impulsive phase of a long-duration M-class solar flare. The 50 s …
View article: A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158
A Data-driven Magnetohydrodynamic Simulation of the 2011 February 15 Coronal Mass Ejection from Active Region NOAA 11158 Open
We present a boundary data-driven magnetohydrodynamic (MHD) simulation of the 2011 February 15 coronal mass ejection (CME) event of Active Region NOAA 11158. The simulation is driven at the lower boundary with an electric field derived fro…
View article: A data-driven MHD simulation of the 2011-02-15 coronal mass ejection from Active Region NOAA 11158
A data-driven MHD simulation of the 2011-02-15 coronal mass ejection from Active Region NOAA 11158 Open
We present a boundary data-driven magneto-hydrodynamic (MHD) simulation of the 2011-02-15 coronal mass ejection (CME) event of Active Region (AR) NOAA 11158. The simulation is driven at the lower boundary with an electric field derived fro…
View article: Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST
Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST Open
We present high-resolution observations of a C4.1-class solar flare (SOL2023-05-03T20:53) in AR 13293 from the Visible Spectro-Polarimeter (ViSP) and Visible Broadband Imager (VBI) instruments at the DKIST. The fast cadence, good resolutio…
View article: Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST
Photospheric Pore Rotation Associated with a C-class Flare from Spectropolarimetric Observations with DKIST Open
We present high-resolution observations of a C4.1-class solar flare (SOL2023-05-03T20:53) in AR 13293 from the ViSP and VBI instruments at the DKIST. The fast cadence, good resolution, and high polarimetric sensitivity of ViSP data provide…
View article: The Relationships among Solar Flare Impulsiveness, Energy Release, and Ribbon Development
The Relationships among Solar Flare Impulsiveness, Energy Release, and Ribbon Development Open
We develop the impulsiveness index, a new classification system for solar flares using the Solar Dynamics Observatory/Extreme Ultraviolet Experiment 304 Å Sun-as-a-star light curves. Impulsiveness classifies events based on the duration an…
View article: Inferring Fundamental Properties of the Flare Current Sheet Using Flare Ribbons: Oscillations in the Reconnection Flux Rates
Inferring Fundamental Properties of the Flare Current Sheet Using Flare Ribbons: Oscillations in the Reconnection Flux Rates Open
Magnetic reconnection is understood to be the main physical process that facilitates the transformation of magnetic energy into heat, motion, and particle acceleration during solar eruptions. Yet, observational constraints on reconnection …
View article: The relationships among solar flare impulsiveness, energy release, and ribbon development
The relationships among solar flare impulsiveness, energy release, and ribbon development Open
We develop the impulsiveness index, a new classification system for solar flares using the SDO/EVE 304 Å Sun-as-a-star light curves. Impulsiveness classifies events based on the duration and intensity of the initial high-energy deposition …
View article: Inferring Fundamental Properties of the Flare Current Sheet Using Flare Ribbons: Oscillations in the Reconnection Flux Rates
Inferring Fundamental Properties of the Flare Current Sheet Using Flare Ribbons: Oscillations in the Reconnection Flux Rates Open
Magnetic reconnection is understood to be the main physical process that facilitates the transformation of magnetic energy into heat, motion, and particle acceleration during solar eruptions. Yet, observational constraints on reconnection …
View article: Large-scale Coronal Dimming Foreshadowing a Solar Eruption on 2011 October 1
Large-scale Coronal Dimming Foreshadowing a Solar Eruption on 2011 October 1 Open
Understanding large-scale solar eruptions requires detailed investigation of the entire system’s evolution, including the magnetic environment enveloping the source region and searches for precursor activity prior to event onset. We combin…
View article: A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares
A Database of Magnetic and Thermodynamic Properties of Confined and Eruptive Solar Flares Open
Solar flares sometimes lead to coronal mass ejections that directly affect Earth's environment. However, a large fraction of flares, including on solar-type stars, are confined flares. What are the differences in physical properties betwee…
View article: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region Open
We investigate the thermal, kinematic, and magnetic structure of small-scale heating events in an emerging flux region (EFR). We use high-resolution multiline observations (including Ca ii 8542 Å, Ca ii K, and the Fe i 6301 Å line pair) of…
View article: A Database of Magnetic and Thermodynamic Properties of Confined And Eruptive Solar Flares
A Database of Magnetic and Thermodynamic Properties of Confined And Eruptive Solar Flares Open
Solar flares sometimes lead to coronal mass ejections that directly affect the Earth's environment. However, a large fraction of flares, including on solar-type stars, are confined flares. What are the differences in physical properties be…
View article: Quantifying Poynting Flux in the Quiet Sun Photosphere
Quantifying Poynting Flux in the Quiet Sun Photosphere Open
Poynting flux is the flux of magnetic energy, which is responsible for chromospheric and coronal heating in the solar atmosphere. It is defined as a cross product of the electric and magnetic fields, and in ideal MHD conditions it can be e…
View article: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region Open
We investigate the thermal, kinematic and magnetic structure of small-scale heating events in an emerging flux region (EFR). We use high-resolution multi-line observations (including Ca II 8542~Å, Ca II K, and Fe I 6301~Åline pair) of an E…