Observations and modeling of D-region ionospheric response of Annular Solar Eclipse on December 26, 2019, using VLF signal amplitude and phase variation
Solar eclipse is a unique phenomenon that produces an orderly disturbance in the ionosphere within a specific time frame. It provides us an opportunity to understand the ionospheric response due to its systematic variation during an eclipse. The amplitude and phase of a Very Low Frequency (VLF) sign...
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| Veröffentlicht in: | Astrophysics and space science 2023-03, Vol.368 (3), p.19, Article 19 |
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| creator | Ghosh, Soujan Chowdhury, Swati Kundu, Subrata Biswas, Sagardweep Dawn, Arjun Ray, Suman Choudhury, Asit K. Bari, Md. Wasimul Bhowmick, Debashis Manna, Souvik Mondal, Sushanta K. Chakrabarti, Sonali Maiti, Rajkumar Das, Ram C. Basak, Tamal Chakrabarti, Sandip K. |
| description | Solar eclipse is a unique phenomenon that produces an orderly disturbance in the ionosphere within a specific time frame. It provides us an opportunity to understand the ionospheric response due to its systematic variation during an eclipse. The amplitude and phase of a Very Low Frequency (VLF) signal carry the response of lower ionospheric perturbation due to the varying solar radiation impinging on Earth. During the Annular Solar Eclipse on December 26, 2019, (ASE2019), Indian Centre for Space Physics (ICSP), Kolkata, India conducted a nationwide VLF radio signal monitoring campaign to obtain the amplitude and phase variations of propagating VLF signal from fourteen different locations across India. The signal amplitude and phase profile exhibit unique profiles at these locations. These profiles in the VLF signal during ASE2019 are explained using the Long Wavelength Propagation Capability (LWPC) code and the modeled variation of solar disk obscuration by the moon. Furthermore, the lower ionospheric electron density (
N
e
) computed from the model is in agreement with the observed lower ionospheric conditions. |
| doi_str_mv | 10.1007/s10509-023-04179-1 |
| format | Article |
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N
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) computed from the model is in agreement with the observed lower ionospheric conditions.</description><identifier>ISSN: 0004-640X</identifier><identifier>EISSN: 1572-946X</identifier><identifier>DOI: 10.1007/s10509-023-04179-1</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Amplitudes ; Astrobiology ; Astronomy ; Astrophysics ; Astrophysics and Astroparticles ; Cosmology ; D region ; Electron density ; Ionosphere ; Ionospheric conditions ; Ionospheric electron density ; Ionospheric electrons ; Ionospheric models ; Observations and Techniques ; Occultation ; Perturbation ; Physics ; Physics and Astronomy ; Radio signals ; Signal monitoring ; Solar eclipses ; Solar radiation ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Very Low Frequencies ; Wave propagation</subject><ispartof>Astrophysics and space science, 2023-03, Vol.368 (3), p.19, Article 19</ispartof><rights>The Author(s), under exclusive licence to Springer Nature B.V. 2023. Springer Nature or its licensor (e.g. a society or other partner) holds exclusive rights to this article under a publishing agreement with the author(s) or other rightsholder(s); author self-archiving of the accepted manuscript version of this article is solely governed by the terms of such publishing agreement and applicable law.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c319t-8e93621050cb9b6a1e3debafb599056af009981f41afc7685537b90bebbf21d83</citedby><cites>FETCH-LOGICAL-c319t-8e93621050cb9b6a1e3debafb599056af009981f41afc7685537b90bebbf21d83</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s10509-023-04179-1$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s10509-023-04179-1$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,778,782,27911,27912,41475,42544,51306</link.rule.ids></links><search><creatorcontrib>Ghosh, Soujan</creatorcontrib><creatorcontrib>Chowdhury, Swati</creatorcontrib><creatorcontrib>Kundu, Subrata</creatorcontrib><creatorcontrib>Biswas, Sagardweep</creatorcontrib><creatorcontrib>Dawn, Arjun</creatorcontrib><creatorcontrib>Ray, Suman</creatorcontrib><creatorcontrib>Choudhury, Asit K.</creatorcontrib><creatorcontrib>Bari, Md. Wasimul</creatorcontrib><creatorcontrib>Bhowmick, Debashis</creatorcontrib><creatorcontrib>Manna, Souvik</creatorcontrib><creatorcontrib>Mondal, Sushanta K.</creatorcontrib><creatorcontrib>Chakrabarti, Sonali</creatorcontrib><creatorcontrib>Maiti, Rajkumar</creatorcontrib><creatorcontrib>Das, Ram C.</creatorcontrib><creatorcontrib>Basak, Tamal</creatorcontrib><creatorcontrib>Chakrabarti, Sandip K.</creatorcontrib><title>Observations and modeling of D-region ionospheric response of Annular Solar Eclipse on December 26, 2019, using VLF signal amplitude and phase variation</title><title>Astrophysics and space science</title><addtitle>Astrophys Space Sci</addtitle><description>Solar eclipse is a unique phenomenon that produces an orderly disturbance in the ionosphere within a specific time frame. It provides us an opportunity to understand the ionospheric response due to its systematic variation during an eclipse. The amplitude and phase of a Very Low Frequency (VLF) signal carry the response of lower ionospheric perturbation due to the varying solar radiation impinging on Earth. During the Annular Solar Eclipse on December 26, 2019, (ASE2019), Indian Centre for Space Physics (ICSP), Kolkata, India conducted a nationwide VLF radio signal monitoring campaign to obtain the amplitude and phase variations of propagating VLF signal from fourteen different locations across India. The signal amplitude and phase profile exhibit unique profiles at these locations. These profiles in the VLF signal during ASE2019 are explained using the Long Wavelength Propagation Capability (LWPC) code and the modeled variation of solar disk obscuration by the moon. Furthermore, the lower ionospheric electron density (
N
e
) computed from the model is in agreement with the observed lower ionospheric conditions.</description><subject>Amplitudes</subject><subject>Astrobiology</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Cosmology</subject><subject>D region</subject><subject>Electron density</subject><subject>Ionosphere</subject><subject>Ionospheric conditions</subject><subject>Ionospheric electron density</subject><subject>Ionospheric electrons</subject><subject>Ionospheric models</subject><subject>Observations and Techniques</subject><subject>Occultation</subject><subject>Perturbation</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Radio signals</subject><subject>Signal monitoring</subject><subject>Solar eclipses</subject><subject>Solar radiation</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Very Low Frequencies</subject><subject>Wave propagation</subject><issn>0004-640X</issn><issn>1572-946X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNp9kctKAzEUhoMoWKsv4CrgttEkc82ytFaFQhde6C4kM2emKXMz6RR8Ex_XTEdw5yIJ4Xz_f87hR-iW0XtGafLgGI2oIJQHhIYsEYSdoQmLEk5EGG_P0YRSGpI4pNtLdOXc3n9FLJIJ-t5oB_aoDqZtHFZNjus2h8o0JW4LvCQWSl_B_rSu24E1GbbgOg_DAMybpq-Uxa_tcD9mlemGQoOXkEGtwWIezzCnTMxw7wbXj_UKO1M2qsKq7ipz6HM49e12ykuPyprTMNfoolCVg5vfd4reV49vi2ey3jy9LOZrkgVMHEgKIoj5sH2mhY4VgyAHrQodCUGjWBV-UZGyImSqyJI4jaIg0YJq0LrgLE-DKbobfTvbfvbgDnLf9taP5yRPUkF5mAahp_hIZbZ1zkIhO2tqZb8ko3JIQI4JSJ-APCUgmRcFo8h5uCnB_ln_o_oB48mJ_g</recordid><startdate>20230301</startdate><enddate>20230301</enddate><creator>Ghosh, Soujan</creator><creator>Chowdhury, Swati</creator><creator>Kundu, Subrata</creator><creator>Biswas, Sagardweep</creator><creator>Dawn, Arjun</creator><creator>Ray, Suman</creator><creator>Choudhury, Asit K.</creator><creator>Bari, Md. 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Wasimul</au><au>Bhowmick, Debashis</au><au>Manna, Souvik</au><au>Mondal, Sushanta K.</au><au>Chakrabarti, Sonali</au><au>Maiti, Rajkumar</au><au>Das, Ram C.</au><au>Basak, Tamal</au><au>Chakrabarti, Sandip K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Observations and modeling of D-region ionospheric response of Annular Solar Eclipse on December 26, 2019, using VLF signal amplitude and phase variation</atitle><jtitle>Astrophysics and space science</jtitle><stitle>Astrophys Space Sci</stitle><date>2023-03-01</date><risdate>2023</risdate><volume>368</volume><issue>3</issue><spage>19</spage><pages>19-</pages><artnum>19</artnum><issn>0004-640X</issn><eissn>1572-946X</eissn><abstract>Solar eclipse is a unique phenomenon that produces an orderly disturbance in the ionosphere within a specific time frame. It provides us an opportunity to understand the ionospheric response due to its systematic variation during an eclipse. The amplitude and phase of a Very Low Frequency (VLF) signal carry the response of lower ionospheric perturbation due to the varying solar radiation impinging on Earth. During the Annular Solar Eclipse on December 26, 2019, (ASE2019), Indian Centre for Space Physics (ICSP), Kolkata, India conducted a nationwide VLF radio signal monitoring campaign to obtain the amplitude and phase variations of propagating VLF signal from fourteen different locations across India. The signal amplitude and phase profile exhibit unique profiles at these locations. These profiles in the VLF signal during ASE2019 are explained using the Long Wavelength Propagation Capability (LWPC) code and the modeled variation of solar disk obscuration by the moon. Furthermore, the lower ionospheric electron density (
N
e
) computed from the model is in agreement with the observed lower ionospheric conditions.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s10509-023-04179-1</doi></addata></record> |
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| subjects | Amplitudes Astrobiology Astronomy Astrophysics Astrophysics and Astroparticles Cosmology D region Electron density Ionosphere Ionospheric conditions Ionospheric electron density Ionospheric electrons Ionospheric models Observations and Techniques Occultation Perturbation Physics Physics and Astronomy Radio signals Signal monitoring Solar eclipses Solar radiation Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Very Low Frequencies Wave propagation |
| title | Observations and modeling of D-region ionospheric response of Annular Solar Eclipse on December 26, 2019, using VLF signal amplitude and phase variation |
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