Owens Valley Solar Arrays: Difference between revisions

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<big>Owens Valley Solar Arrays (OVSA) is a university-led radio facility dedicated to solar astrophysics and space weather research. Located in the Owens Valley Radio Observatory (OVRO) near Big Pine, California, the operations of OVSA include the Expanded Owens Valley Solar Array (EOVSA) observing in the microwave regime (1-18 GHz), as well as the solar and space weather aspects of the newly commissioned Long Wavelength Array at the Owens Valley Radio Observatory (OVRO-LWA), which observes in the meter-decameter wavelength regime (13-87 MHz). Please refer to [https://ovsa.njit.edu/ our home page] for more general descriptions of the facility. This wiki serves as the site for OVSA documentation.  </big>


<big>[http://ovsa.njit.edu/ EOVSA] (Expanded Owens Valley Solar Array) is a new solar-dedicated radio interferometer operated by the New Jersey Institute of Technology. This wiki serves as the site for EOVSA documentation.  </big>
{| class="wikitable" style="border: none;"
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| ''Operation of OVSA is supported by the National Science Foundation under Grant AGS-2436999. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation.''
| [[File:NSF.jpg|70px]]
|}
 
== Latest OVSA Science 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.]
 
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[[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]]
A study by [https://iopscience.iop.org/article/10.3847/2041-8213/adf063 Y. 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 Yuankun Kou (Nanjing University); Edited by B. Chen. Posted on August 2, 2025.]
 
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We welcome contributions at all times. Please refer to the [[OVSA Science Highlights]] page for author guidelines and a complete list of highlights.
 
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== OVSA Publications ==
Our collection of publications that utilize OVSA data is available at [https://ui.adsabs.harvard.edu/public-libraries/eQ7HfPkySqydu-B8BCt6QQ this NASA/ADS Library]. If you have a paper that is missing from this library, please email Bin Chen (bin.chen [at] njit.edu).
<!--
; 2025
: Lesovoi, S.V., Gary, D.E., Globa, M.V., Ivanov, E.F. (2025), Solar Physics 300, 23. [https://doi.org/10.1007/s11207-025-02433-z "On a Possible Scenario of Solar Coherent Bursts"]
: Xu, Y., Wang, M., Cao, A., Ji, K., Yurchyshyn, V., Qiu, J., Yu, S., Shen, J., & Cao, W. (2025), The Astrophysical Journal Letters, 979, L43. [https://iopscience.iop.org/article/10.3847/2041-8213/ada9e4 "High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons"]
 
; 2024
: Collier, H., Hayes, L. A., Yu, S., Battaglia, A. F., Ashfield, W., Polito, V., Harra, L. K., & Krucker, S. (2024), arXiv e-prints, arXiv:2402.10546. [https://ui.adsabs.harvard.edu/abs/2024arXiv240210546C “Localising pulsations in the hard X-ray and microwave emission of an X-class flare”]
: Saqri, J., Veronig, A. M., Battaglia, A. F., Dickson, E. C. M., Gary, D. E., & Krucker, S. (2024), Astronomy and Astrophysics, 683, A41. [https://ui.adsabs.harvard.edu/abs/2024A&A...683A..41S "Efficiency of solar microflares in accelerating electrons when rooted in a sunspot"]
: Wei, Y., Chen, B., Yu, S., Wang, H., Zhang, Y., & Glesener, L. (2024), The Astrophysical Journal, 964, 174. [https://iopscience-iop-org.libdb.njit.edu:8443/article/10.3847/1538-4357/ad2e8f "Episodic Energy Release during the Main and Post-impulsive Phases of a Solar Flare"]
 
; 2023
: Tan, B., Yan, Y., Huang, J., Zhang, Y., Tan, C., & Zhu, X. (2023), Advances in Space Research, 72, 5563. [https://ui.adsabs.harvard.edu/abs/2023AdSpR..72.5563T "The physics of solar spectral imaging observations in dm-cm wavelengths and the application on space weather"]
 
: Li, D., Li, Z., Shi, F., Su, Y., Chen, W., Yu, F., Li, C., Qiu, Y., Huang, Y., & Ning, Z. (2023), Astronomy and Astrophysics, 680, L15. [https://ui.adsabs.harvard.edu/abs/2023A&A...680L..15L "Observational signature of continuously operating drivers of decayless kink oscillation"]
 
: Wang, M., Chen, B., Yu, S., Gary, D. E., Lee, J., Wang, H., & Cohen, C. (2023), The Astrophysical Journal, 954, 32. [https://ui.adsabs.harvard.edu/abs/2023ApJ...954...32W "The Solar Origin of an In Situ Type III Radio Burst Event"]
 
: Gary, D. E. (2023), Annual Review of Astronomy and Astrophysics, 61, 427. [https://ui.adsabs.harvard.edu/abs/2023ARA&A..61..427G "New Insights from Imaging Spectroscopy of Solar Radio Emission"]
 
: Nita, G. M., Fleishman, G. D., Kuznetsov, A. A., Anfinogentov, S. A., Stupishin, A. G., Kontar, E. P., Schonfeld, S. J., Klimchuk, J. A., & Gary, D. E. (2023), The Astrophysical Journal Supplement Series, 267, 6. [https://ui.adsabs.harvard.edu/abs/2023ApJS..267....6N "Data-constrained Solar Modeling with GX Simulator"]
 
: Song, D.-C., Tian, J., Li, Y., Ding, M. D., Su, Y., Yu, S., Hong, J., Qiu, Y., Rao, S., Liu, X., Li, Q., Chen, X., Li, C., & Fang, C. (2023), The Astrophysical Journal, 952, L6. [https://ui.adsabs.harvard.edu/abs/2023ApJ...952L...6S "Spectral Observations and Modeling of a Solar White-light Flare Observed by CHASE"]
 
: Mondal, S., Chen, B., & Yu, S. (2023), The Astrophysical Journal, 949, 56. [https://ui.adsabs.harvard.edu/abs/2023ApJ...949...56M "Multifrequency Microwave Imaging of Weak Transients from the Quiet Solar Corona"]
 
: Kontar, E. P., Emslie, A. G., Motorina, G. G., & Dennis, B. R. (2023), The Astrophysical Journal, 947, L13. [https://ui.adsabs.harvard.edu/abs/2023ApJ...947L..13K "The Efficiency of Electron Acceleration during the Impulsive Phase of a Solar Flare"]
 
: Saqri, J., Veronig, A. M., Dickson, E. C. M., Podladchikova, T., Warmuth, A., Xiao, H., Gary, D. E., Battaglia, A. F., & Krucker, S. (2023), Astronomy and Astrophysics, 672, A23. [https://ui.adsabs.harvard.edu/abs/2023A&A...672A..23S "Multi-point study of the energy release and impulsive CME dynamics in an eruptive C7 flare"]
; 2022
 
: Kou, Y., Cheng, X., Wang, Y., Yu, S., Chen, B., Kontar, E. P., & Ding, M. (2022), Nature Communications, 13, 7680. [https://ui.adsabs.harvard.edu/abs/2022NatCo..13.7680K "Microwave imaging of quasi-periodic pulsations at flare current sheet"]
 
: Chertok, I. M. (2022), Monthly Notices of the Royal Astronomical Society, 517, 2709. [https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.2709C "On some features of the solar proton event on 2021 October 28 - GLE73"]
 
: Lörinčík, J., Polito, V., De Pontieu, B., Yu, S., & Freij, N. (2022), Frontiers in Astronomy and Space Sciences, 9, 334. [https://ui.adsabs.harvard.edu/abs/2022FrASS...940945L "Rapid variations of Si IV spectra in a flare observed by interface region imaging spectrograph at a sub-second cadence"]
 
: Klein, K.-L., Musset, S., Vilmer, N., Briand, C., Krucker, S., Francesco Battaglia, A., Dresing, N., Palmroos, C., & Gary, D. E. (2022), Astronomy and Astrophysics, 663, A173. [https://ui.adsabs.harvard.edu/abs/2022A&A...663A.173K "The relativistic solar particle event on 28 October 2021: Evidence of particle acceleration within and escape from the solar corona"]
 
: Fleishman, G. D., Nita, G. M., Chen, B., Yu, S., & Gary, D. E. (2022), Nature, 606, 674. [https://ui.adsabs.harvard.edu/abs/2022Natur.606..674F "Solar flare accelerates nearly all electrons in a large coronal volume"]
 
: Li, X., Guo, F., Chen, B., Shen, C., & Glesener, L. (2022), The Astrophysical Journal, 932, 92. [https://ui.adsabs.harvard.edu/abs/2022ApJ...932...92L "Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare"]
 
: Zhang, J., Chen, B., Yu, S., Tian, H., Wei, Y., Chen, H., Tan, G., Luo, Y., & Chen, X. (2022), The Astrophysical Journal, 932, 53. [https://ui.adsabs.harvard.edu/abs/2022ApJ...932...53Z "Implications for Additional Plasma Heating Driving the Extreme-ultraviolet Late Phase of a Solar Flare with Microwave Imaging Spectroscopy"]
 
: Liu, N., Jing, J., Xu, Y., & Wang, H. (2022), The Astrophysical Journal, 930, 154. [https://ui.adsabs.harvard.edu/abs/2022ApJ...930..154L "Multi-instrument Comparative Study of Temperature, Number Density, and Emission Measure during the Precursor Phase of a Solar Flare"]
 
: López, F. M., Giménez de Castro, C. G., Mandrini, C. H., Simões, P. J. A., Cristiani, G. D., Gary, D. E., Francile, C., & Démoulin, P. (2022), Astronomy and Astrophysics, 657, A51. [https://ui.adsabs.harvard.edu/abs/2022A&A...657A..51L "A solar flare driven by thermal conduction observed in mid-infrared"]
 
: Unverferth, J., & Longcope, D. (2021), The Astrophysical Journal, 923, 248. [https://ui.adsabs.harvard.edu/abs/2021ApJ...923..248U "Examining Flux Tube Interactions as a Cause of Sub-alfvénic Outflow"]
;2021
 
: Wei, Y., Chen, B., Yu, S., Wang, H., Jing, J., & Gary, D. E. (2021), The Astrophysical Journal, 923, 213. [https://ui.adsabs.harvard.edu/abs/2021ApJ...923..213W "Coronal Magnetic Field Measurements along a Partially Erupting Filament in a Solar Flare"]
 
: Jing, J., Inoue, S., Lee, J., Li, Q., Nita, G. M., Xu, Y., Liu, C., Gary, D. E., & Wang, H. (2021), The Astrophysical Journal, 922, 108. [https://ui.adsabs.harvard.edu/abs/2021ApJ...922..108J "Understanding the Initiation of the M2.4 Flare on 2017 July 14"]
 
: Battaglia, A. F., Saqri, J., Massa, P., Perracchione, E., Dickson, E. C. M., Xiao, H., Veronig, A. M., Warmuth, A., Battaglia, M., Hurford, G. J., Meuris, A., Limousin, O., Etesi, L., Maloney, S. A., Schwartz, R. A., Kuhar, M., Schuller, F., Senthamizh Pavai, V., Musset, S., Ryan, D. F., Kleint, L., Piana, M., Massone, A. M., Benvenuto, F., Sylwester, J., Litwicka, M., Stȩślicki, M., Mrozek, T., Vilmer, N., Fárník, F., Kašparová, J., Mann, G., Gallagher, P. T., Dennis, B. R., Csillaghy, A., Benz, A. O., & Krucker, S. (2021), Astronomy and Astrophysics, 656, A4. [https://ui.adsabs.harvard.edu/abs/2021A&A...656A...4B "STIX X-ray microflare observations during the Solar Orbiter commissioning phase"]
 
: Shaik, S. B., & Gary, D. E. (2021), The Astrophysical Journal, 919, 44. [https://ui.adsabs.harvard.edu/abs/2021ApJ...919...44S "Implications of Flat Optically Thick Microwave Spectra in Solar Flares for Source Size and Morphology"]
 
: Kocharov, L., Omodei, N., Mishev, A., Pesce-Rollins, M., Longo, F., Yu, S., Gary, D. E., Vainio, R., & Usoskin, I. (2021), The Astrophysical Journal, 915, 12. [https://ui.adsabs.harvard.edu/abs/2021ApJ...915...12K "Multiple Sources of Solar High-energy Protons"]
 
: Chen, B., Battaglia, M., Krucker, S., Reeves, K. K., & Glesener, L. (2021), The Astrophysical Journal, 908, L55. [https://ui.adsabs.harvard.edu/abs/2021ApJ...908L..55C "Energetic Electron Distribution of the Coronal Acceleration Region: First Results from Joint Microwave and Hard X-Ray Imaging Spectroscopy"]
 
: Chhabra, S., Gary, D. E., Hallinan, G., Anderson, M. M., Chen, B., Greenhill, L. J., & Price, D. C. (2021), The Astrophysical Journal, 906, 132. [https://ui.adsabs.harvard.edu/abs/2021ApJ...906..132C "Imaging Spectroscopy of CME-associated Solar Radio Bursts using OVRO-LWA"]
;2020 and earlier
 
: Reeves, K. K., Polito, V., Chen, B., Galan, G., Yu, S., Liu, W., & Li, G. (2020), The Astrophysical Journal, 905, 165. [https://ui.adsabs.harvard.edu/abs/2020ApJ...905..165R "Hot Plasma Flows and Oscillations in the Loop-top Region During the 2017 September 10 X8.2 Solar Flare"]
 
: Nindos, A. (2020), Frontiers in Astronomy and Space Sciences, 7, 57. [https://ui.adsabs.harvard.edu/abs/2020FrASS...7...57N "Incoherent Solar Radio Emission"]
 
: Yu, S., Chen, B., Reeves, K. K., Gary, D. E., Musset, S., Fleishman, G. D., Nita, G. M., & Glesener, L. (2020), The Astrophysical Journal, 900, 17. [https://ui.adsabs.harvard.edu/abs/2020ApJ...900...17Y "Magnetic Reconnection during the Post-impulsive Phase of a Long-duration Solar Flare: Bidirectional Outflows as a Cause of Microwave and X-Ray Bursts"]
 
: Chen, B., Yu, S., Reeves, K. K., & Gary, D. E. (2020), The Astrophysical Journal, 895, L50. [https://ui.adsabs.harvard.edu/abs/2020ApJ...895L..50C "Microwave Spectral Imaging of an Erupting Magnetic Flux Rope: Implications for the Standard Solar Flare Model in Three Dimensions"]
 
: Kuroda, N., Fleishman, G. D., Gary, D. E., Nita, G. M., Chen, B., & Yu, S. (2020), Frontiers in Astronomy and Space Sciences, 7, 22. [https://ui.adsabs.harvard.edu/abs/2020FrASS...7...22K "Evolution of Flare-accelerated Electrons Quantified by Spatially Resolved Analysis"]
 
: Glesener, L., Krucker, S., Duncan, J., Hannah, I. G., Grefenstette, B. W., Chen, B., Smith, D. M., White, S. M., & Hudson, H. (2020), The Astrophysical Journal, 891, L34. [https://ui.adsabs.harvard.edu/abs/2020ApJ...891L..34G "Accelerated Electrons Observed Down to <7 keV in a NuSTAR Solar Microflare"]
 
: Karlický, M., Chen, B., Gary, D. E., Kašparová, J., & Rybák, J. (2020), The Astrophysical Journal, 889, 72. [https://ui.adsabs.harvard.edu/abs/2020ApJ...889...72K "Drifting Pulsation Structure at the Very Beginning of the 2017 September 10 Limb Flare"]
 
: Fleishman, G. D., Gary, D. E., Chen, B., Kuroda, N., Yu, S., & Nita, G. M. (2020), Science, 367, 278. [https://ui.adsabs.harvard.edu/abs/2020Sci...367..278F "Decay of the coronal magnetic field can release sufficient energy to power a solar flare"]
 
: Chen, B., Shen, C., Gary, D. E., Reeves, K. K., Fleishman, G. D., Yu, S., Guo, F., Krucker, S., Lin, J., Nita, G. M., & Kong, X. (2020), Nature Astronomy, 4, 1140. [https://ui.adsabs.harvard.edu/abs/2020NatAs...4.1140C "Measurement of magnetic field and relativistic electrons along a solar flare current sheet"]
 
: Lee, J. (2018), Journal of Astronomy and Space Sciences, 35, 211. [https://ui.adsabs.harvard.edu/abs/2018JASS...35..211L "Analysis of Solar Microwave Burst Spectrum, I. Nonuniform Magnetic Field"]
 
: Gary, D. E., Bastian, T. S., Chen, B., Fleishman, G. D., & Glesener, L. (2018), Science with a Next Generation Very Large Array, 517, 99. [https://ui.adsabs.harvard.edu/abs/2018ASPC..517...99G "Radio Observations of Solar Flares"]
 
: Polito, V., Dudík, J., Kašparová, J., Dzifčáková, E., Reeves, K. K., Testa, P., & Chen, B. (2018), The Astrophysical Journal, 864, 63. [https://ui.adsabs.harvard.edu/abs/2018ApJ...864...63P "Broad Non-Gaussian Fe XXIV Line Profiles in the Impulsive Phase of the 2017 September 10 X8.3-class Flare Observed by Hinode/EIS"]
 
: Gary, D. E., Chen, B., Dennis, B. R., Fleishman, G. D., Hurford, G. J., Krucker, S., McTiernan, J. M., Nita, G. M., Shih, A. Y., White, S. M., & Yu, S. (2018), The Astrophysical Journal, 863, 83. [https://ui.adsabs.harvard.edu/abs/2018ApJ...863...83G "Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare"]
 
: Fleishman, G. D., Nita, G. M., Kuroda, N., Jia, S., Tong, K., Wen, R. R., & Zhizhuo, Z. (2018), The Astrophysical Journal, 859, 17. [https://ui.adsabs.harvard.edu/abs/2018ApJ...859...17F "Revealing the Evolution of Non-thermal Electrons in Solar Flares Using 3D Modeling"]
 
: Kuroda, N., Gary, D. E., Wang, H., Fleishman, G. D., Nita, G. M., & Jing, J. (2018), The Astrophysical Journal, 852, 32. [https://ui.adsabs.harvard.edu/abs/2018ApJ...852...32K "Three-dimensional Forward-fit Modeling of the Hard X-Ray and Microwave Emissions of the 2015 June 22 M6.5 Flare"]
 
: Wang, H., Liu, C., Ahn, K., Xu, Y., Jing, J., Deng, N., Huang, N., Liu, R., Kusano, K., Fleishman, G. D., Gary, D. E., & Cao, W. (2017), Nature Astronomy, 1, 0085. [https://ui.adsabs.harvard.edu/abs/2017NatAs...1E..85W "High-resolution observations of flare precursors in the low solar atmosphere"]
 
: Nita, G. M., Hickish, J., MacMahon, D., & Gary, D. E. (2016), Journal of Astronomical Instrumentation, 5, 1641009-7366. [https://ui.adsabs.harvard.edu/abs/2016JAI.....541009N "EOVSA Implementation of a Spectral Kurtosis Correlator for Transient Detection and Classification"]
 
: Nita, G. M., & Gary, D. E. (2016), Journal of Geophysical Research (Space Physics), 121, 7353. [https://ui.adsabs.harvard.edu/abs/2016JGRA..121.7353N "Measurement of duration and signal-to-noise ratio of astronomical transients using a Spectral Kurtosis spectrometer"]
 
: Wang, Z., Gary, D. E., Fleishman, G. D., & White, S. M. (2015), The Astrophysical Journal, 805, 93. [https://ui.adsabs.harvard.edu/abs/2015ApJ...805...93W "Coronal Magnetography of a Simulated Solar Active Region from Microwave Imaging Spectropolarimetry"]
 
: Gary, D. E., Fleishman, G. D., & Nita, G. M. (2013), Solar Physics, 288, 549. [https://ui.adsabs.harvard.edu/abs/2013SoPh..288..549G "Magnetography of Solar Flaring Loops with Microwave Imaging Spectropolarimetry"]
-->
 
== EOVSA Flare List ==
 
* [https://ovsa.njit.edu/flarelist Query EOVSA Flare list]
* List of EOVSA flares in separate years: [[2025]], [[2024]], [[2023]], [[2022]], [[2021]], [[2020]], [[2019]], [[2017]]
 
== OVSA Observing ==
 
=== OVSA Weekly Observing Reports ===
* 2025
** Q4: [https://drive.google.com/file/d/1a_1yGUCdTDf5WXMy9I7vQHF_aYFGtMQT/view?usp=sharing 09/30-10/06], [https://drive.google.com/file/d/1rMHmGEVSgtjPIUp79eRQIx36Sh9Yim0S/view?usp=drive_link 10/07-10/13], [https://drive.google.com/file/d/1etXFQmVuUThH80lc61Fa3i8fCPwZ3OPM/view?usp=drive_link 10/14-10/20], [https://drive.google.com/file/d/12Wxmls11_mHTOTl_zdv5G1q1gomOsIXz/view?usp=drive_link 10/21-10/27], [https://drive.google.com/file/d/1pkNgGQh8ph6RvFsL1IR7ig8vN7tAlXS9/view?usp=drive_link 10/28-11/03], [https://drive.google.com/file/d/1PyGC6ixUoGwE1zMdm8ylIh1g51dAIHkQ/view?usp=drive_link 11/04-11/10], [https://drive.google.com/file/d/1s5b_hkhyL_eaHPbMAWUPq8XWpjD5Glln/view?usp=drive_link 11/11-11/17], [https://drive.google.com/file/d/1g_e-iWS-Qgs80d_xYzeEz_GKKc5P-Rax/view?usp=drive_link 11/18-11/24], [https://drive.google.com/file/d/1zmUzY82MwJpkols8GGGQZXz4wWixW_9q/view?usp=sharing 11/25-12/01]
** Q3: [https://drive.google.com/file/d/1NLJpfehI7XiyNQc_9L69H9xrXn_LsCQM/view?usp=drive_link 08/26-09/01], [https://drive.google.com/file/d/1QiD9rk_DocXT1F3aRl3L49AAyaNaR9d1/view?usp=drive_link 09/02-09/08], [https://drive.google.com/file/d/1O2oGCAAnBX4YOmbWsra14zPxk2t7CQXn/view?usp=drive_link 09/09-09/15], [https://drive.google.com/file/d/1C-CF_OW8EqQflTPzceRzAyX3cRq8hKJ6/view?usp=drive_link 09/16-09/22], [https://drive.google.com/file/d/14ci0XpFu-kqPbcoPliUjnDNOHAoXi1vH/view?usp=drive_link 09/23-09/29]
 
=== OVSA Scientist on Duty ===
* Scientist on Duty (SoD): OVSA team members take turns and serve as a SoD to work with our onsite observatory staff on day-to-day observing. They are also responsible for monitoring solar activities and ensuring that the data we collect is of high quality.
* SoD observing logs ([https://drive.google.com/drive/folders/1q6-0Z9B0CPFutuTqzmeheEUSJM3tEL2o?usp=drive_link directory to all logs and weekly reports]):
** 2024: [https://docs.google.com/document/d/1QDWw5y4HpcE7CSpzXwftMqQT4FDgNJj-6fRrgWrqdug/edit?usp=sharing May (and before that)], [https://docs.google.com/document/d/1Rh2gYBV2E454xVYEv8jx5IXKd1N2Z05ns4dhI2XCE08/edit?usp=sharing June], [https://docs.google.com/document/d/1beUpp6rgwjqSxKbuHzXIR9hhPrGyi0j-SjtEIeav9Vg/edit?usp=sharing July], [https://docs.google.com/document/d/1pSzUXW5gd-4cZAR-gglTUVM_J2UHMa4wYJ2AzD4cdEo/edit?usp=sharing August], [https://docs.google.com/document/d/18pArAP0kRDhXHbty_y3TtrygmWkC2oLn-UD7njIpRIo/edit?usp=sharing September], [https://docs.google.com/document/d/1Qt6vhrqPAOG7W5Y_tLiod_QgNR1FDyzRxQcg6_oJQd4/edit?usp=sharing October], [https://docs.google.com/document/d/1pv9-Wne80FCrg0J5BkjOafmof_s3jlnc9HwyzWkIBfU/edit?usp=sharing November], [https://docs.google.com/document/d/1O5svOVwQZbUON1GMR_8nBR5LAL0M8RM2_zWW4oeBiLk/edit?usp=sharing December]
** 2025: [https://docs.google.com/document/d/1pUdSRyWgQa2py1PSLa3CKs_DDqL_SOgx6MMIp4cPnpk/edit?usp=sharing January], [https://docs.google.com/document/d/18cnIAaeM8UBiYPtsQn7g6TM8mjr57blSoY9l-6ShhwQ/edit?usp=sharing February], [https://docs.google.com/document/d/1k60i7nabWltnU38I7fGS2uq2-FUe5TMAKcM1BeLIRdY/edit?usp=sharing March], [https://docs.google.com/document/d/1CMaXBtA1ULNFbzuawYirP913A6dTa68cbYk2a7knirI/edit?usp=sharing April], [https://docs.google.com/document/d/13Kr8lYfFN9bzgFvCJi6nBUxbQHa3_eTgfjwaCUn3vCs/edit?tab=t.0 May], [https://docs.google.com/document/d/1ptGvQiB6SPgzJ-I6IgJ4bKK-3GPK-4LBpq7BG6sFPSg/edit?usp=sharing June], [https://docs.google.com/document/d/1XrOonOdwrkSDSWT2CwvzIaw7aRxBA4Sba1GCMRmkDZk/edit?usp=sharing July], [https://docs.google.com/document/d/1MzKkL8cPaBLNDOuws4U0ATuTN7kVaaeX4dUp0cga3vo/edit?usp=sharing August], [https://docs.google.com/document/d/14JHnHLZiDTqtK_cmaHgRevKksHuqijBQcMo1zcrz98k/edit?usp=sharing September], [https://docs.google.com/document/d/1RypoU6RtXVIdak_ESgabEK1Gp8XG7Tok2kHhPNZ3G4g/edit?usp=sharing October], [https://docs.google.com/document/d/1fQDS7mTQSnSfvTYozY6vXRrW_mleTf1vABTZhwYDKdw/edit?usp=sharing November]
 
* SoD instructions:
** Daily routines: see [https://docs.google.com/document/d/1_iGnMRRrvb85Z0vT8-LzgQmCOKDSATEuQ0vTsn2C-dc/edit?usp=sharing SoD Routines] for detailed instructions.
** Instructions for [[making quick-look flare spectrograms and movies]]
 
=== EOVSA Observing Log ===
[[2016 November]]; [[2016 December| December]]
 
[[2017 January]]; [[2017 February | February]]; [[2017 March | March]]; [[2017 April | April]]; [[2017 May | May]]; [[2017 June | June]];
[[2017 July | July]]; [[2017 August | August]]; [[2017 September | September]]; [[2017 October | October]]; [[2017 November | November]]; [[2017 December | December]]
 
[[2018 January]]; [[2018 February | February]]; [[2018 March | March]]; [[2018 April | April]]; [[2018 May | May]]; [[2018 June | June]];
[[2018 July | July]]; [[2018 August | August]]; [[2018 September | September]]; [[2018 October | October]]; [[2018 November | November]]; [[2018 December | December]]
 
[[2019 January]]; [[2019 February | February]]; [[2019 March | March]]; [[2019 April | April]]; [[2019 May | May]]; [[2019 June | June]];
[[2019 July | July]]; [[2019 August | August]]; [[2019 September | September]]; [[2019 October | October]]; [[2019 November | November]]; [[2019 December | December]]
 
[[2020 January]]; [[2020 February | February]]; [[2020 March | March]]; [[2020 April | April]]; [[2020 May | May]]; [[2020 June | June]];
[[2020 July | July]]; [[2020 August | August]]; [[2020 September | September]]; [[2020 October | October]]; [[2020 November | November]]; [[2020 December | December]]
 
[[2021 January]]; [[2021 February | February]]; [[2021 March | March]]; [[2021 April | April]]; [[2021 May | May]]; [[2021 June | June]];
[[2021 July | July]]; [[2021 August | August]]; [[2021 September | September]]; [[2021 October | October]]; [[2021 November | November]]; [[2021 December | December]]
 
[[2022 SQL Outage]]
 
[[2023 January]]; [[2023 February | February]]; [[2023 March | March]]; [[2023 April | April]]; [[2023 May | May]]; [[2023 June | June]];
[[2023 July | July]]; [[2023 August | August]]; [[2023 September | September]]; [[2023 October | October]]; [[2023 November | November]]; [[2023 December | December]]
 
[[2024 January]]; [[2024 February | February]]; [[2024 March | March]]; [[2024 April | April]]; [[2024 May |May]]; [[2024 June | June]]; [[2024 July | July]];  [[2024 August | August]];
[[2024 September | September]]; [[2024 October | October]]; [[2024 November | November]]; [[2024 December | December]]
 
[[2025 January]]; [[2025 February | February]]; [[2025 March | March]]; [[2025 April | April]]; [[2025 May |May]]; [[2025 June | June]]; [[2025 July | July]];  [[2025 August | August]];
[[2025 September | September]]; [[2025 October | October]]; [[2025 November | November]]; [[2025 December | December]]
 
== Using OVSA Data  ==
* <big>[[EOVSA Data Products]]</big>: An introduction to standard EOVSA spectrogram and spectral image products with example scripts for reading and plotting.
* <big>[[OVRO-LWA Solar Data Products]]</big>: An introduction to OVRO-LWA solar spectrogram and spectral image products with example scripts for reading and plotting.
* <big>[[OVSA Data Policy]]</big>: Policy for using OVSA data products.
* <big>Analysis Software</big>: These are for in-depth use of EOVSA data (from calibrated visibilities) and tools for quantitative analysis.   
** [https://github.com/suncasa/suncasa SunCASA] A wrapper around [https://casa.nrao.edu/ CASA (the Common Astronomy Software Applications package)] for synthesis imaging and visualizing solar spectral imaging data. CASA is one of the leading software tool for "supporting the data post-processing needs of the next generation of radio astronomical telescopes such as ALMA and VLA", an international effort led by the [https://public.nrao.edu/ National Radio Astronomy Observatory]. The current version of CASA uses Python (2.7) interface. More information about CASA can be found on [https://casa.nrao.edu/ NRAO's CASA website ]. Note, CASA is available ONLY on UNIX-BASED PLATFORMS (and therefore, so is SunCASA).
** [https://github.com/Gelu-Nita/GSFIT GSFIT] A IDL-widget(GUI)-based spectral fitting package called gsfit, which provides a user-friendly display of EOVSA image cubes and an interface to fast fitting codes (via platform-dependent shared-object libraries).
** [https://github.com/suncasa/pygsfit pyGSFIT] A Python-widget(pyQT)-based spectral fitting package, which provides a user-friendly display of EOVSA image cubes, spatially resolved spectra, and an interface to scipy-based fitting codes.
** [[Spectrogram Software]]
** [[Mapping Software]]
* <big>Data Analysis Guides (for those who start from raw data) </big>
<!--** <big>[[EOVSA Data Analysis Tutorial 2022]]</big> and <big>[https://colab.research.google.com/drive/19NQb6Emb9HvKX4QHq9ZYCP3RM6nT7sDL#scrollTo=cLdDVptBGG-X EOVSA Workspace]</big> at [https://sphere.boulder.swri.edu/ SPHERE 2022 Workshop]-->
<!--** <big>[https://colab.research.google.com/drive/1lSLLxgOG6b8kgu9Sk6kSKvrViyubnXG6?usp=sharing#scrollTo=xbXyyLmCFCGL EOVSA Data Analysis Tutorial at RHESSI 19 Workshop]</big>-->
<!--** <big>[[EOVSA Data Analysis Tutorial]]</big> at [http://rhessi18.umn.edu/ RHESSI XVIII Workshop]-->
<!-- ** [[Self-Calibrating Flare Data]] Example script and guides for self-calibrating EOVSA flare data (to be completed)-->
<!-- ** [[Imaging]] -->
<!-- ** [[Flare Imaging]] -->
**[[Tohban Guide to Self Calibration and Imaging for EOVSA]] Step-to-step guide for manually making images from raw visibility data.
**[[EOVSA flare pipeline]] Description of the EOVSA flare pipeline and tutorial for running it to produce quicklook images.
<!-- ** [[Imaging]] -->
<!-- ** [[Flare Imaging]] -->
 
* <big>EOVSA Modeling Guide</big>
**[[GX Simulator]]
 
* Other helpful links
** [https://casaguides.nrao.edu CASA Guides]
** [http://www.lmsal.com/solarsoft/ SolarSoft IDL]
** [http://www.atnf.csiro.au/computing/software/miriad/userguide/userhtml.html Miriad Guides]
** [https://sites.google.com/site/fgscodes/ Fast Gyrosynchrotron Codes (Alexey Kuznetsov's website)]
** [[Basic GitHub Tutorial]]
 
<!--* <big>[[EOVSA Imaging Workshop]]</big>-->
* <big>[[Full Disk Simulations]]</big>
* <big>[[All-Day Synthesis Issues]]</big>
* <big>[[Analyzing Pre-2017 Data]]</big>
* <big>[[Fixing Pipeline Problems pre-2021-Feb-07]]</big>


== EOVSA Documentation ==
== EOVSA Documentation ==
Line 9: Line 254:
** [[Dealing with Radio Frequency Interference]]
** [[Dealing with Radio Frequency Interference]]
** [[Switching between 200 MHz and 300 MHz Correlator]]
** [[Switching between 200 MHz and 300 MHz Correlator]]
** [[Observing in "Fast" Mode]]


* <big>Computer-Network</big>
* <big>Computer-Network</big>
Line 47: Line 293:
* <big>[[Starburst]]</big>
* <big>[[Starburst]]</big>


== Using EOVSA Data  ==
* <big>[[EOVSA Data products]]</big>
* <big>Analysis Software</big>
** [https://github.com/suncasa/suncasa SunCASA] A wrapper around [https://casa.nrao.edu/ CASA (the Common Astronomy Software Applications package)] for synthesis imaging and visualizing solar spectral imaging data. CASA is one of the leading software tool for "supporting the data post-processing needs of the next generation of radio astronomical telescopes such as ALMA and VLA", an international effort led by the [https://public.nrao.edu/ National Radio Astronomy Observatory]. The current version of CASA uses Python (2.7) interface. More information about CASA can be found on [https://casa.nrao.edu/ NRAO's CASA website ]. Note, CASA is available ONLY on UNIX-BASED PLATFORMS (and therefore, so is SunCASA).
** [https://github.com/Gelu-Nita/GSFIT GSFIT] A IDL-widget(GUI)-based spectral fitting package called gsfit, which provides a user-friendly display of EOVSA image cubes and an interface to fast fitting codes (via platform-dependent shared-object libraries).
** [[Spectrogram Software]]
** [[Mapping Software]]
* <big>Data Analysis Guides</big>
** <big>[[EOVSA Data Analysis Tutorial 2022]]</big> and <big>[https://colab.research.google.com/drive/19NQb6Emb9HvKX4QHq9ZYCP3RM6nT7sDL#scrollTo=cLdDVptBGG-X EOVSA Workspace]</big> at [https://sphere.boulder.swri.edu/ SPHERE 2022 Workshop]
** <big>[https://colab.research.google.com/drive/1lSLLxgOG6b8kgu9Sk6kSKvrViyubnXG6?usp=sharing#scrollTo=xbXyyLmCFCGL EOVSA Data Analysis Tutorial at RHESSI 19 Workshop]</big>
** <big>[[EOVSA Data Analysis Tutorial]]</big> at [http://rhessi18.umn.edu/ RHESSI XVIII Workshop]
** [[Self-Calibrating Flare Data]] Example script and guides for self-calibrating EOVSA flare data (to be completed)
<!-- ** [[Imaging]] -->
<!-- ** [[Flare Imaging]] -->
**[[IDB flare pipeline]] Tutorial to run the flare pipeline for quicklook images
<!-- ** [[Imaging]] -->
<!-- ** [[Flare Imaging]] -->
* <big>EOVSA Modeling Guide</big>
**[[GX Simulator]]
* Other helpful links
** [https://casaguides.nrao.edu CASA Guides]
** [http://www.lmsal.com/solarsoft/ SolarSoft IDL]
** [http://www.atnf.csiro.au/computing/software/miriad/userguide/userhtml.html Miriad Guides]
** [https://sites.google.com/site/fgscodes/ Fast Gyrosynchrotron Codes (Alexey Kuznetsov's website)]
** [[Basic GitHub Tutorial]]
<!--* <big>[[EOVSA Imaging Workshop]]</big>-->
* <big>[[Full Disk Simulations]]</big>
* <big>[[All-Day Synthesis Issues]]</big>
* <big>[[Analyzing Pre-2017 Data]]</big>
* <big>[[Fixing Pipeline Problems pre-2021-Feb-07]]</big>


== System Software ==
== EOVSA System Software ==


* LabVIEW software
* LabVIEW software
Line 87: Line 300:
* [[Python3 Code Installation]]
* [[Python3 Code Installation]]


== Observing Log ==
==OVRO-LWA Solar-Dedicated Spectroscopic Imager==
[[2016 November]]; [[2016 December| December]]
The OVRO-LWA (Owens Valley Radio Observatory Long Wavelength Array) has recently been upgraded to include a solar-dedicated beam and two solar imaging modes (slow visibilities of 352 antennas with a 10-s cadence, and fast visibilities of 48 antennas with a 0.1-s cadence).  The large collecting area and excellent calibration provide unprecedented high-sensitivity imaging of the quiet Sun and bursts.  The array is currently in commissioning and observations are not yet continuous, but they are becoming more so.  See the daily realtime data at http://ovsa.njit.edu/status.php for '''real-time display of the spectrogram and a selection of images''', both updated on a 1-min cadence.


[[2017 January]]; [[2017 February | February]]; [[2017 March | March]]; [[2017 April | April]]; [[2017 May | May]]; [[2017 June | June]];
===Solar-Dedicated Modes===
[[2017 July | July]]; [[2017 August | August]]; [[2017 September | September]]; [[2017 October | October]]; [[2017 November | November]]; [[2017 December | December]]
* Beamformer: The OVRO-LWA beamformer uses the 256 antennas in the core region to form a synthesized beam of more than 1 degree in size that tracks the Sun from sunrise to sunset. This permits a continuous record of the full-Stokes total flux (without spatial resolution) of the Sun (a dynamic spectrum) with 24 kHz frequency resolution (3072 frequencies from 13.4-86.9 MHz) and as low as 1 ms time resolution.


[[2018 January]]; [[2018 February | February]]; [[2018 March | March]]; [[2018 April | April]]; [[2018 May | May]]; [[2018 June | June]];
* Standard Interferometric Imaging (also known as "Slow Visibilities"): In this mode, the entire 352-element array is interferometrically correlated to provide visibilities for imaging at all 3072 frequencies at 10-s time resolution.  This is ideal for imaging quiet Sun and slowly-varying emission such as coronal mass ejections and active region variability.
[[2018 July | July]]; [[2018 August | August]]; [[2018 September | September]]; [[2018 October | October]]; [[2018 November | November]]; [[2018 December | December]]


[[2019 January]]; [[2019 February | February]]; [[2019 March | March]]; [[2019 April | April]]; [[2019 May | May]]; [[2019 June | June]];
* Bursty Interferometric Imaging (also known as "Fast Visibilities"): In this mode, a subset of 48 antennas (chosen to include mainly outer antennas to maintain good spatial resolution) is interferometrically correlated to provide visibilities for imaging at 768 frequencies (96 kHz frequency resolution) at 0.1-s time resolution.  This is ideal for imaging rapidly varying emission such as type II and type III bursts as well as many other solar spectral fine structures.
[[2019 July | July]]; [[2019 August | August]]; [[2019 September | September]]; [[2019 October | October]]; [[2019 November | November]]; [[2019 December | December]]


[[2020 January]]; [[2020 February | February]]; [[2020 March | March]]; [[2020 April | April]]; [[2020 May | May]]; [[2020 June | June]];
===Data Access===
[[2020 July | July]]; [[2020 August | August]]; [[2020 September | September]]; [[2020 October | October]]; [[2020 November | November]]; [[2020 December | December]]
* OVRO-LWA solar data release v1.0 is available! Please refer to the [[OVRO-LWA Data Products]] page for more information.


[[2021 January]]; [[2021 February | February]]; [[2021 March | March]]; [[2021 April | April]]; [[2021 May | May]]; [[2021 June | June]];
===OVRO-LWA Operation Notes===
[[2021 July | July]]; [[2021 August | August]]; [[2021 September | September]]; [[2021 October | October]]; [[2021 November | November]]; [[2021 December | December]]


[[2022 SQL Outage]]
[[OVRO-LWA Operation Notes]]


== Tohbans ==
== Tohbans ==
Line 114: Line 324:


[[Owen's Notes]]
[[Owen's Notes]]
[[Caius' Notes]]


[[Tohban EOVSA Imaging Tutorial A-Z]]
[[Tohban EOVSA Imaging Tutorial A-Z]]
[[Tohban OVRO-LWA Imaging Tutorial]]


[[Tohban Guide to Self Calibration and Imaging for EOVSA]]
[[Tohban Guide to Self Calibration and Imaging for EOVSA]]
Line 121: Line 335:
[[Guide to Upgrade SolarSoft(SSW)]]
[[Guide to Upgrade SolarSoft(SSW)]]


== EOVSA Flare List ==
[[Star Pointing Notes]]
 
See [https://docs.google.com/spreadsheets/d/1P8jHuDRF93dMflU6RMQcsJqVepD9vFkPkofV8Imj4xA/edit?usp=sharing this link] for a list of EOVSA flares as a Google Spreadsheet.
 
[[Recent Flare List (2021-)]]
 
[http://ovsa.njit.edu/jay/rd_db.php An older link] is available at the EOVSA website.
 
== EOVSA Publications ==
Here is a (partial) list of publications that utilize EOVSA data. See also the collection of EOVSA publications at [https://ui.adsabs.harvard.edu/public-libraries/eQ7HfPkySqydu-B8BCt6QQ this NASA/ADS Library].
; 2023
: [https://ui.adsabs.harvard.edu/abs/2023arXiv230107840M/abstract Mondal, S., Chen, B. & Yu, S. (2023) ApJ, submitted] ''Multifrequency microwave imaging of weak transients from the quiet solar corona''
; 2022
: [https://ui.adsabs.harvard.edu/abs/2022FrASS...940945L/abstract Lörinčík et al (2022) Frontiers, 9, 1] ''Rapid variations of Si IV spectra in a flare observed by interface region imaging spectrograph at a sub-second cadence''
: [https://ui.adsabs.harvard.edu/abs/2022NatCo..13.7680K/abstract Kou et al. (2022) Nature Communications 13, 7680] ''Microwave imaging of quasi-periodic pulsations at flare current sheet''
: [https://ui.adsabs.harvard.edu/abs/2022Natur.606..674F/abstract Fleishman et al. (2022) Nature 606, 674] ''Solar flare accelerates nearly all electrons in a large coronal volume''
: [https://ui.adsabs.harvard.edu/abs/2022ApJ...932...92L/abstract Li, X., et al., (2022) ApJ, 932, 92] ''Modeling Electron Acceleration and Transport in the Early Impulsive Phase of the 2017 September 10th Solar Flare''
: [https://ui.adsabs.harvard.edu/abs/2022ApJ...930..154L/abstract Liu, N., et al., (2022), ApJ, 930, 154] ''Multi-instrument Comparative Study of Temperature, Number Density, and Emission Measure during the Precursor Phase of a Solar Flare''
: [https://ui.adsabs.harvard.edu/abs/2022arXiv220503518Z/abstract Zhang et al. (2022), ApJ, 932, 53] ''Implications for additional plasma heating driving the extreme-ultraviolet late phase of a solar flare with microwave imaging spectroscopy''
: [https://ui.adsabs.harvard.edu/abs/2022A%26A...657A..51L/abstract Lopez et al. (2021), A&A, 657, A51] ''A solar flare driven by thermal conduction observed in mid-infrared''
; 2021
: [https://ui.adsabs.harvard.edu/abs/2021ApJ...923..213W/abstract Wei et al. (2021), ApJ, 923, 213] ''Coronal Magnetic Field Measurements along a Partially Erupting Filament in a Solar Flare''
: [https://ui.adsabs.harvard.edu/abs/2021ApJ...919...44S/abstract Shaik & Gary (2021), ApJ, 919, 44] ''Implications of Flat Optically Thick Microwave Spectra in Solar Flares for Source Size and Morphology''
: [https://ui.adsabs.harvard.edu/abs/2021ApJ...915...12K/abstract Kocharov et al. (2021), ApJ, 915, 12] ''Multiple Sources of Solar High-energy Protons''
: [https://ui.adsabs.harvard.edu/abs/2021ApJ...908L..55C/abstract Chen et al. (2021), ApJL, 908, L55] ''Energetic Electron Distribution of the Coronal Acceleration Region: First results from Joint Microwave and Hard X-ray Imaging Spectroscopy''
: [https://ui.adsabs.harvard.edu/abs/2021ApJ...906..132C/abstract Chhabra et al. (2021), ApJ, 906, 132] ''Imaging Spectroscopy of CME-Associated Solar Radio Bursts''
; 2020
: [https://ui.adsabs.harvard.edu/abs/2020ApJ...905..165R/abstract Reeves et al. (2020), ApJ, 905, 165] ''Hot Plasma Flows and Oscillations in the Loop-top Region During the September 10 2017 X8.2 Solar Flare''
: [https://ui.adsabs.harvard.edu/abs/2020ApJ...900...17Y/abstract Yu et al. (2020), ApJ, 900, 17] ''Magnetic Reconnection During the Post Impulsive Phase of the X8.2 Solar Flare: Bi-Directional Outflows as a Cause of Microwave and X-ray Bursts''
: [https://ui.adsabs.harvard.edu/abs/2020NatAs...4.1140C/abstract Chen et al. (2020b), Nature Astronomy, 4, 1140] ''Measurement of magnetic field and relativistic electrons along a solar flare current sheet''
: [https://ui.adsabs.harvard.edu/abs/2020ApJ...895L..50C/abstract Chen et al. (2020a), ApJL, 895, 50] ''Microwave Spectral Imaging of an Erupting Magnetic Flux Rope: Implications for the Standard Solar Flare Model in Three Dimensions''
: [https://ui.adsabs.harvard.edu/abs/2020FrASS...7...22K/abstract Kuroda et al. (2020), Frontiers, 7, 22] ''Evolution of Flare-accelerated Electrons Quantified by Spatially Resolved Analysis''
: [https://ui.adsabs.harvard.edu/abs/2020ApJ...891L..34G/abstract Glesener et al. (2020), ApJL, 891, 34] ''Accelerated Electrons Observed Down to <7 keV in a NuSTAR Solar Microflare''
: [https://ui.adsabs.harvard.edu/abs/2020ApJ...889...72K/abstract Karlicky at al. (2020), ApJ, 889, 72] ''Drifting Pulsation Structure at the Very Beginning of the 2017 September 10 Limb Flare''
: [https://ui.adsabs.harvard.edu/abs/2020Sci...367..278F/abstract Fleishman et al. (2020), Science, 367, 278] ''Decay of the coronal magnetic field can release sufficient energy to power a solar flare''
: [https://ui.adsabs.harvard.edu/abs/2020AAS...23538501G/abstract Gary et al. (2020), BAAS 52, 385.01] [https://aas235-aas.ipostersessions.com/default.aspx?s=97-69-9E-4B-34-19-68-53-1B-C6-21-0C-16-1C-5C-82&guestview=true Direct link to AAS iPoster] ''A new view of the solar atmosphere: daily full-disk multifrequency radio images from EOVSA''
; 2018
: [https://ui.adsabs.harvard.edu/#abs/2018ApJ...864...63P/abstract Polito et al. (2018), ApJ, 864, 63] ''Broad Non-Gaussian Fe XXIV Line Profiles in the Impulsive Phase of the 2017 September 10 X8.3-class Flare Observed by Hinode/EIS''
: [https://ui.adsabs.harvard.edu/#abs/2018ApJ...863...83G/abstract Gary et al. (2018), ApJ, 863, 83] ''Microwave and Hard X-Ray Observations of the 2017 September 10 Solar Limb Flare''
: [https://ui.adsabs.harvard.edu/#abs/2018ApJ...852...32K/abstract Kuroda et al. (2018), ApJ, 852, 32] ''Three-dimensional Forward-fit Modeling of the Hard X-ray and the Microwave Emissions of the 2015 June 22 M6.5 flare''
; 2017
: [https://ui.adsabs.harvard.edu/abs/2017NatAs...1E..85W/abstract Wang et al. (2017), Nature Astronomy, 1, 85] ''High-resolution observations of flare precursors in the low solar atmosphere''
; 2016
: [https://ui.adsabs.harvard.edu/abs/2016JAI.....541009N/abstract Nita et al. (2016), J. Astron. Instr., 5, 1641009-7366] ''EOVSA Implementation of a Spectral Kurtosis Correlator for Transient Detection and Classification''


== VLA Flare List and Publications ==
== VLA Flare List and Publications ==
Line 181: Line 352:
* [https://ui.adsabs.harvard.edu/abs/2014ApJ...794..149C/abstract Chen et al. (2014), ApJ, 794, 149] ''Direct Evidence of an Eruptive, Filament-hosting Magnetic Flux Rope Leading to a Fast Solar Coronal Mass Ejection''
* [https://ui.adsabs.harvard.edu/abs/2014ApJ...794..149C/abstract Chen et al. (2014), ApJ, 794, 149] ''Direct Evidence of an Eruptive, Filament-hosting Magnetic Flux Rope Leading to a Fast Solar Coronal Mass Ejection''
* [https://ui.adsabs.harvard.edu/abs/2013ApJ...763L..21C/abstract Chen et al. (2013), ApJL, 763, 21] ''Tracing Electron Beams in the Sun's Corona with Radio Dynamic Imaging Spectroscopy''
* [https://ui.adsabs.harvard.edu/abs/2013ApJ...763L..21C/abstract Chen et al. (2013), ApJL, 763, 21] ''Tracing Electron Beams in the Sun's Corona with Radio Dynamic Imaging Spectroscopy''
==Radio Data from Around The Heliosphere==
* [http://ovsa.njit.edu//wiki/index.php/Radio_Data_from_Around_the_World#Radio_Data_Access '' Radio Data '']
==Radio Astronomy Lecture Notes==
Here is a link to the [[Radio Astronomy Lecture Notes]] adapted from the Phys728: Radio Astronomy graduate-level course Prof. Dale Gary taught at NJIT until Spring 2019.

Latest revision as of 21:37, 5 December 2025

Owens Valley Solar Arrays (OVSA) is a university-led radio facility dedicated to solar astrophysics and space weather research. Located in the Owens Valley Radio Observatory (OVRO) near Big Pine, California, the operations of OVSA include the Expanded Owens Valley Solar Array (EOVSA) observing in the microwave regime (1-18 GHz), as well as the solar and space weather aspects of the newly commissioned Long Wavelength Array at the Owens Valley Radio Observatory (OVRO-LWA), which observes in the meter-decameter wavelength regime (13-87 MHz). Please refer to our home page for more general descriptions of the facility. This wiki serves as the site for OVSA documentation.

Operation of OVSA is supported by the National Science Foundation under Grant AGS-2436999. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. NSF.jpg

Latest OVSA Science Highlights

OVSA Science Highlight No. 6: Detection of Radio Gyroresonance Emission from a CME

Cme 20240309.jpeg

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?

Cme mfr.jpeg

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

Crab solar conjunction.jpeg

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

Cold flare.jpeg

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

SEP illustration gemini.jpeg

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

Solar eruption nasa.jpeg

A study by Y. 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 Yuankun Kou (Nanjing University); Edited by B. Chen. Posted on August 2, 2025.]

We welcome contributions at all times. Please refer to the OVSA Science Highlights page for author guidelines and a complete list of highlights.

OVSA Publications

Our collection of publications that utilize OVSA data is available at this NASA/ADS Library. If you have a paper that is missing from this library, please email Bin Chen (bin.chen [at] njit.edu).

EOVSA Flare List

OVSA Observing

OVSA Weekly Observing Reports

OVSA Scientist on Duty

EOVSA Observing Log

2016 November; December

2017 January; February; March; April; May; June; July; August; September; October; November; December

2018 January; February; March; April; May; June; July; August; September; October; November; December

2019 January; February; March; April; May; June; July; August; September; October; November; December

2020 January; February; March; April; May; June; July; August; September; October; November; December

2021 January; February; March; April; May; June; July; August; September; October; November; December

2022 SQL Outage

2023 January; February; March; April; May; June; July; August; September; October; November; December

2024 January; February; March; April; May; June; July; August; September; October; November; December

2025 January; February; March; April; May; June; July; August; September; October; November; December

Using OVSA Data

  • EOVSA Data Products: An introduction to standard EOVSA spectrogram and spectral image products with example scripts for reading and plotting.
  • OVRO-LWA Solar Data Products: An introduction to OVRO-LWA solar spectrogram and spectral image products with example scripts for reading and plotting.
  • OVSA Data Policy: Policy for using OVSA data products.
  • Analysis Software: These are for in-depth use of EOVSA data (from calibrated visibilities) and tools for quantitative analysis.
    • SunCASA A wrapper around CASA (the Common Astronomy Software Applications package) for synthesis imaging and visualizing solar spectral imaging data. CASA is one of the leading software tool for "supporting the data post-processing needs of the next generation of radio astronomical telescopes such as ALMA and VLA", an international effort led by the National Radio Astronomy Observatory. The current version of CASA uses Python (2.7) interface. More information about CASA can be found on NRAO's CASA website . Note, CASA is available ONLY on UNIX-BASED PLATFORMS (and therefore, so is SunCASA).
    • GSFIT A IDL-widget(GUI)-based spectral fitting package called gsfit, which provides a user-friendly display of EOVSA image cubes and an interface to fast fitting codes (via platform-dependent shared-object libraries).
    • pyGSFIT A Python-widget(pyQT)-based spectral fitting package, which provides a user-friendly display of EOVSA image cubes, spatially resolved spectra, and an interface to scipy-based fitting codes.
    • Spectrogram Software
    • Mapping Software
  • Data Analysis Guides (for those who start from raw data)

EOVSA Documentation


EOVSA System Software

OVRO-LWA Solar-Dedicated Spectroscopic Imager

The OVRO-LWA (Owens Valley Radio Observatory Long Wavelength Array) has recently been upgraded to include a solar-dedicated beam and two solar imaging modes (slow visibilities of 352 antennas with a 10-s cadence, and fast visibilities of 48 antennas with a 0.1-s cadence). The large collecting area and excellent calibration provide unprecedented high-sensitivity imaging of the quiet Sun and bursts. The array is currently in commissioning and observations are not yet continuous, but they are becoming more so. See the daily realtime data at http://ovsa.njit.edu/status.php for real-time display of the spectrogram and a selection of images, both updated on a 1-min cadence.

Solar-Dedicated Modes

  • Beamformer: The OVRO-LWA beamformer uses the 256 antennas in the core region to form a synthesized beam of more than 1 degree in size that tracks the Sun from sunrise to sunset. This permits a continuous record of the full-Stokes total flux (without spatial resolution) of the Sun (a dynamic spectrum) with 24 kHz frequency resolution (3072 frequencies from 13.4-86.9 MHz) and as low as 1 ms time resolution.
  • Standard Interferometric Imaging (also known as "Slow Visibilities"): In this mode, the entire 352-element array is interferometrically correlated to provide visibilities for imaging at all 3072 frequencies at 10-s time resolution. This is ideal for imaging quiet Sun and slowly-varying emission such as coronal mass ejections and active region variability.
  • Bursty Interferometric Imaging (also known as "Fast Visibilities"): In this mode, a subset of 48 antennas (chosen to include mainly outer antennas to maintain good spatial resolution) is interferometrically correlated to provide visibilities for imaging at 768 frequencies (96 kHz frequency resolution) at 0.1-s time resolution. This is ideal for imaging rapidly varying emission such as type II and type III bursts as well as many other solar spectral fine structures.

Data Access

  • OVRO-LWA solar data release v1.0 is available! Please refer to the OVRO-LWA Data Products page for more information.

OVRO-LWA Operation Notes

OVRO-LWA Operation Notes

Tohbans

Trouble Shooting Guide

Tohban Records

Owen's Notes

Caius' Notes

Tohban EOVSA Imaging Tutorial A-Z

Tohban OVRO-LWA Imaging Tutorial

Tohban Guide to Self Calibration and Imaging for EOVSA

Guide to Upgrade SolarSoft(SSW)

Star Pointing Notes

VLA Flare List and Publications

See this link for a list of flare observations made by the Karl G. Jansky Very Large Array (VLA). Below is a partial list of publications that utilize VLA solar data (see also this NASA/ADS Library).

Radio Data from Around The Heliosphere

Radio Astronomy Lecture Notes

Here is a link to the Radio Astronomy Lecture Notes adapted from the Phys728: Radio Astronomy graduate-level course Prof. Dale Gary taught at NJIT until Spring 2019.

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