OVSA Science Highlights: Difference between revisions
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==For Authors== | ==For Authors== | ||
We welcome submissions for all works that utilize OVSA data. Please see [https://docs.google.com/document/d/1ygn7BrU8IKu-6Q00_MCZTeswLZFXOl9TKU342-u_tCU/edit?usp=sharing the Author Guidelines] for submission guidance. | We welcome submissions for all works that utilize OVSA data. Please see [https://docs.google.com/document/d/1ygn7BrU8IKu-6Q00_MCZTeswLZFXOl9TKU342-u_tCU/edit?usp=sharing the Author Guidelines] for submission guidance. Here is a [https://docs.google.com/document/d/16OyzDDefSHJKMWO607MuVzKipX0sQJaz6Lr8yIOMqSM/edit?tab=t.0 Google Doc template] based on a published OVSA highlight. | ||
== | ==All Highlights== | ||
[[OVSA Science Highlight No. 6: Detection of Radio Gyroresonance Emission from a CME]] | |||
[[File:cme_20240309.jpeg|left|100px]] | |||
[https://arxiv.org/abs/2509.16453 This study] reports the first possible detection of thermal gyroresonance emission from a CME. This breakthrough offers a new potential method for measuring the magnetic field of CMEs. [Contributed by Surajit Mondal (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 26, 2025.] | |||
[[OVSA Science Highlight | <div style="clear: both;"></div> | ||
[[OVSA Science Highlight No. 5: Is CME's Magnetic Flux Conserved?]] | |||
[[File:cme_mfr.jpeg|left|100px]] | |||
According to [https://iopscience.iop.org/article/10.3847/2041-8213/adfa71 this study], the answer is "probably yes." The conclusion is made by using ultrabroadband radio imaging spectroscopy to derive the magnetic field evolution of an erupting CME from the low to middle corona. [Contributed by Xingyao Chen (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 19, 2025.] | |||
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[[OVSA Science Highlight No. 4: When the Sun Meets the Crab]] | |||
[[File:crab_solar_conjunction.jpeg|left|100px]] | |||
When the Crab Nebula passes behind the Sun each June, radio telescopes can catch its distorted signals, providing a rare way to probe turbulence in the Sun’s extended atmosphere out to more than 10 solar radii. [Contributed by Peijin Zhang (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 11, 2025.] | |||
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[[OVSA Science Highlight No. 3: The First EOVSA "Cold" Solar Flare]] | |||
[[File:cold_flare.jpeg|left|100px]] | |||
[https://iopscience.iop.org/article/10.3847/1538-4357/ade983 This study] takes advantage of EOVSA's microwave imaging spectroscopy capability and multi-wavelength observations to measure the coronal magnetic field and track the flare energy partitioning. The results show ample magnetic free energy to drive efficient electron acceleration, with the energy deposition of nonthermal electrons alone accounting for the observed thermal response, reinforcing cold flares as clean cases of particle-driven heating. [Contributed by Gregory Fleishman (New Jersey Institute of Technology); Edited by B. Chen. Posted on August 20, 2025.] | |||
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[[OVSA Science Highlight No. 2: Two Phases of Impulsive SEP Acceleration]] | |||
[[File:SEP_illustration_gemini.jpeg|left|100px]] | |||
[https://iopscience.iop.org/article/10.3847/1538-4357/adbdd0 M. Wang et al.] analyze a solar energetic particle (SEP) event associated with an eruptive X-class flare and found two distinct impulsive SEP acceleration phases. They are suggested to link to different magnetic reconnection regimes during the eruption, which govern the timing and energy of particles released into interplanetary space. [Contributed by Meiqi Wang (New Jersey Institute of Technology); Edited by B. Chen. Posted on August 19, 2025.] | |||
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[[OVSA Science Highlight No. 1: Microwave Precursor of a Major Solar Eruption]] | |||
[[File:solar_eruption_nasa.jpeg|left|100px]] | [[File:solar_eruption_nasa.jpeg|left|100px]] | ||
A study by [https://iopscience.iop.org/article/10.3847/2041-8213/adf063 Kou et al.] presents the first spatially resolved microwave imaging spectroscopy of the precursor phase of a major solar eruption. The findings reveal that thermal electron emissions dominate during the slow-rise phase, supporting a scenario of moderate magnetic reconnection prior to the flare’s impulsive onset. [Contributed by Y. Kou; Edited by B. Chen. Posted on August 2, 2025.] | A study by [https://iopscience.iop.org/article/10.3847/2041-8213/adf063 Kou et al.] presents the first spatially resolved microwave imaging spectroscopy of the precursor phase of a major solar eruption. The findings reveal that thermal electron emissions dominate during the slow-rise phase, supporting a scenario of moderate magnetic reconnection prior to the flare’s impulsive onset. [Contributed by Y. Kou; Edited by B. Chen. Posted on August 2, 2025.] | ||
Latest revision as of 20:00, 26 September 2025
For Authors
We welcome submissions for all works that utilize OVSA data. Please see the Author Guidelines for submission guidance. Here is a Google Doc template based on a published OVSA highlight.
All Highlights
OVSA Science Highlight No. 6: Detection of Radio Gyroresonance Emission from a CME
This study reports the first possible detection of thermal gyroresonance emission from a CME. This breakthrough offers a new potential method for measuring the magnetic field of CMEs. [Contributed by Surajit Mondal (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 26, 2025.]
OVSA Science Highlight No. 5: Is CME's Magnetic Flux Conserved?
According to this study, the answer is "probably yes." The conclusion is made by using ultrabroadband radio imaging spectroscopy to derive the magnetic field evolution of an erupting CME from the low to middle corona. [Contributed by Xingyao Chen (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 19, 2025.]
OVSA Science Highlight No. 4: When the Sun Meets the Crab
When the Crab Nebula passes behind the Sun each June, radio telescopes can catch its distorted signals, providing a rare way to probe turbulence in the Sun’s extended atmosphere out to more than 10 solar radii. [Contributed by Peijin Zhang (New Jersey Institute of Technology); Edited by B. Chen. Posted on September 11, 2025.]
OVSA Science Highlight No. 3: The First EOVSA "Cold" Solar Flare
This study takes advantage of EOVSA's microwave imaging spectroscopy capability and multi-wavelength observations to measure the coronal magnetic field and track the flare energy partitioning. The results show ample magnetic free energy to drive efficient electron acceleration, with the energy deposition of nonthermal electrons alone accounting for the observed thermal response, reinforcing cold flares as clean cases of particle-driven heating. [Contributed by Gregory Fleishman (New Jersey Institute of Technology); Edited by B. Chen. Posted on August 20, 2025.]
OVSA Science Highlight No. 2: Two Phases of Impulsive SEP Acceleration
M. Wang et al. analyze a solar energetic particle (SEP) event associated with an eruptive X-class flare and found two distinct impulsive SEP acceleration phases. They are suggested to link to different magnetic reconnection regimes during the eruption, which govern the timing and energy of particles released into interplanetary space. [Contributed by Meiqi Wang (New Jersey Institute of Technology); Edited by B. Chen. Posted on August 19, 2025.]
OVSA Science Highlight No. 1: Microwave Precursor of a Major Solar Eruption
A study by Kou et al. presents the first spatially resolved microwave imaging spectroscopy of the precursor phase of a major solar eruption. The findings reveal that thermal electron emissions dominate during the slow-rise phase, supporting a scenario of moderate magnetic reconnection prior to the flare’s impulsive onset. [Contributed by Y. Kou; Edited by B. Chen. Posted on August 2, 2025.]