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Characteristics of Jupiter's X‐Ray Auroral Hot Spot Emissions Using Chandra
To help understand and determine the driver of jovian auroral X‐rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalog we explore dates from December 18, 2000 up to and including September 8, 2019. Us...
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| Published in: | Journal of geophysical research. Space physics 2021-09, Vol.126 (9), p.n/a |
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| creator | Weigt, D. M. Jackman, C. M. Vogt, M. F. Manners, H. Dunn, W. R. Gladstone, G. R. Kraft, R. Branduardi‐Raymont, G. Louis, C. K. McEntee, S. C. |
| description | To help understand and determine the driver of jovian auroral X‐rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalog we explore dates from December 18, 2000 up to and including September 8, 2019. Using a numerical criterion, we characterize the typical and extreme behavior of the concentrated NHS emissions across the catalog. The mean power of the NHS is found to be 1.91 GW with a maximum brightness of 2.02 Rayleighs (R), representing by far the brightest parts of the jovian X‐ray spectrum. We report a statistically significant region of emissions at the NHS center which is always present, the averaged hot spot nucleus (AHSNuc), with mean power of 0.57 GW and inferred average brightness of ∼1.2 R. We use a flux equivalence mapping model to link this distinct region of X‐ray output to a likely source location and find that the majority of mappable NHS photons emanate from the pre‐dusk to pre‐midnight sector, coincident with the dusk flank boundary. A smaller cluster maps to the noon magnetopause boundary, dominated by the AHSNuc, suggesting that there may be multiple drivers of X‐ray emissions. On application of timing analysis techniques (Rayleigh, Monte Carlo, Jackknife), we identify several instances of statistically significant quasi‐periodic oscillations (QPOs) in the NHS photons ranging from ∼2.3 to 36.4 min, suggesting possible links with ultra‐low frequency activity on the magnetopause boundary (e.g., dayside reconnection, Kelvin‐Helmholtz instabilities).
Plain Language Summary
The auroral emissions (northern and southern lights) on Jupiter are the most powerful in our Solar System and have been observed across the electromagnetic spectrum. The cause, or driver, of Jupiter's auroras is still an open question with lots of scientific debate. The solar wind can have an effect, as can Jupiter's volcanic moon Io. The plasma and magnetic field interactions can produce auroras on Jupiter in the X‐ray waveband. These powerful X‐ray emissions can be observed by telescopes like the Chandra X‐ray Observatory (CXO) that orbit Earth. The X‐ray data we analyze here have been found to flash or pulsate at certain periods, spanning the ∼20 years Chandra has observed Jupiter. We use mapping and timing analysis techniques to analyze the entire catalog from the high‐resolution camera on‐board Chandra. We report significant auroral X‐ray regions and pulsations in the No |
| doi_str_mv | 10.1029/2021JA029243 |
| format | article |
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Plain Language Summary
The auroral emissions (northern and southern lights) on Jupiter are the most powerful in our Solar System and have been observed across the electromagnetic spectrum. The cause, or driver, of Jupiter's auroras is still an open question with lots of scientific debate. The solar wind can have an effect, as can Jupiter's volcanic moon Io. The plasma and magnetic field interactions can produce auroras on Jupiter in the X‐ray waveband. These powerful X‐ray emissions can be observed by telescopes like the Chandra X‐ray Observatory (CXO) that orbit Earth. The X‐ray data we analyze here have been found to flash or pulsate at certain periods, spanning the ∼20 years Chandra has observed Jupiter. We use mapping and timing analysis techniques to analyze the entire catalog from the high‐resolution camera on‐board Chandra. We report significant auroral X‐ray regions and pulsations in the North to help us provide an answer for the possible multiple X‐ray drivers.
Key Points
We present the first statistical study looking at the behavior of Jupiter's northern X‐ray auroral hot spot from 20 years of Chandra data
The X‐rays map close to the magnetopause from noon to dusk, with the center of the averaged hot spot emissions mapping to noon
Our analysis suggests that the X‐ray driver(s) may be linked with ultra‐low frequency wave activity along the magnetopause</description><identifier>ISSN: 2169-9380</identifier><identifier>EISSN: 2169-9402</identifier><identifier>DOI: 10.1029/2021JA029243</identifier><language>eng</language><publisher>Washington: Blackwell Publishing Ltd</publisher><subject>aurora ; Auroral emissions ; Auroras ; Brightness ; Hot spots (geology) ; jovian magnetosphere ; Jupiter ; Jupiter atmosphere ; Magnetic fields ; Magnetopause ; magnetosphere ; Mapping ; Mean ; Morphology ; Photons ; Planetary magnetic fields ; Solar system ; Solar wind ; Solar wind effects ; Space telescopes ; Telescopes ; ULF waves ; Wind effects ; X‐ray aurora</subject><ispartof>Journal of geophysical research. Space physics, 2021-09, Vol.126 (9), p.n/a</ispartof><rights>2021. The Authors.</rights><rights>2021. This article is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c3458-c893722f1d697fa6309b1016b26a622780c822ed00cdd027bddb8588e6deb4c3</citedby><cites>FETCH-LOGICAL-c3458-c893722f1d697fa6309b1016b26a622780c822ed00cdd027bddb8588e6deb4c3</cites><orcidid>0000-0002-6620-6357 ; 0000-0002-3276-7420 ; 0000-0003-0060-072X ; 0000-0003-0635-7361 ; 0000-0002-0383-6917 ; 0000-0001-5427-6537 ; 0000-0002-9552-8822 ; 0000-0003-4885-8615</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://onlinelibrary.wiley.com/doi/pdf/10.1029%2F2021JA029243$$EPDF$$P50$$Gwiley$$Hfree_for_read</linktopdf><linktohtml>$$Uhttps://onlinelibrary.wiley.com/doi/full/10.1029%2F2021JA029243$$EHTML$$P50$$Gwiley$$Hfree_for_read</linktohtml><link.rule.ids>315,786,790,27957,27958,50923,51032</link.rule.ids></links><search><creatorcontrib>Weigt, D. M.</creatorcontrib><creatorcontrib>Jackman, C. M.</creatorcontrib><creatorcontrib>Vogt, M. F.</creatorcontrib><creatorcontrib>Manners, H.</creatorcontrib><creatorcontrib>Dunn, W. R.</creatorcontrib><creatorcontrib>Gladstone, G. R.</creatorcontrib><creatorcontrib>Kraft, R.</creatorcontrib><creatorcontrib>Branduardi‐Raymont, G.</creatorcontrib><creatorcontrib>Louis, C. K.</creatorcontrib><creatorcontrib>McEntee, S. C.</creatorcontrib><title>Characteristics of Jupiter's X‐Ray Auroral Hot Spot Emissions Using Chandra</title><title>Journal of geophysical research. Space physics</title><description>To help understand and determine the driver of jovian auroral X‐rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalog we explore dates from December 18, 2000 up to and including September 8, 2019. Using a numerical criterion, we characterize the typical and extreme behavior of the concentrated NHS emissions across the catalog. The mean power of the NHS is found to be 1.91 GW with a maximum brightness of 2.02 Rayleighs (R), representing by far the brightest parts of the jovian X‐ray spectrum. We report a statistically significant region of emissions at the NHS center which is always present, the averaged hot spot nucleus (AHSNuc), with mean power of 0.57 GW and inferred average brightness of ∼1.2 R. We use a flux equivalence mapping model to link this distinct region of X‐ray output to a likely source location and find that the majority of mappable NHS photons emanate from the pre‐dusk to pre‐midnight sector, coincident with the dusk flank boundary. A smaller cluster maps to the noon magnetopause boundary, dominated by the AHSNuc, suggesting that there may be multiple drivers of X‐ray emissions. On application of timing analysis techniques (Rayleigh, Monte Carlo, Jackknife), we identify several instances of statistically significant quasi‐periodic oscillations (QPOs) in the NHS photons ranging from ∼2.3 to 36.4 min, suggesting possible links with ultra‐low frequency activity on the magnetopause boundary (e.g., dayside reconnection, Kelvin‐Helmholtz instabilities).
Plain Language Summary
The auroral emissions (northern and southern lights) on Jupiter are the most powerful in our Solar System and have been observed across the electromagnetic spectrum. The cause, or driver, of Jupiter's auroras is still an open question with lots of scientific debate. The solar wind can have an effect, as can Jupiter's volcanic moon Io. The plasma and magnetic field interactions can produce auroras on Jupiter in the X‐ray waveband. These powerful X‐ray emissions can be observed by telescopes like the Chandra X‐ray Observatory (CXO) that orbit Earth. The X‐ray data we analyze here have been found to flash or pulsate at certain periods, spanning the ∼20 years Chandra has observed Jupiter. We use mapping and timing analysis techniques to analyze the entire catalog from the high‐resolution camera on‐board Chandra. We report significant auroral X‐ray regions and pulsations in the North to help us provide an answer for the possible multiple X‐ray drivers.
Key Points
We present the first statistical study looking at the behavior of Jupiter's northern X‐ray auroral hot spot from 20 years of Chandra data
The X‐rays map close to the magnetopause from noon to dusk, with the center of the averaged hot spot emissions mapping to noon
Our analysis suggests that the X‐ray driver(s) may be linked with ultra‐low frequency wave activity along the magnetopause</description><subject>aurora</subject><subject>Auroral emissions</subject><subject>Auroras</subject><subject>Brightness</subject><subject>Hot spots (geology)</subject><subject>jovian magnetosphere</subject><subject>Jupiter</subject><subject>Jupiter atmosphere</subject><subject>Magnetic fields</subject><subject>Magnetopause</subject><subject>magnetosphere</subject><subject>Mapping</subject><subject>Mean</subject><subject>Morphology</subject><subject>Photons</subject><subject>Planetary magnetic fields</subject><subject>Solar system</subject><subject>Solar wind</subject><subject>Solar wind effects</subject><subject>Space telescopes</subject><subject>Telescopes</subject><subject>ULF waves</subject><subject>Wind effects</subject><subject>X‐ray aurora</subject><issn>2169-9380</issn><issn>2169-9402</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><sourceid>24P</sourceid><sourceid>WIN</sourceid><recordid>eNp9kNFKwzAUhoMoOObufICAF95YTU7aNL0sY26OiTAneFfSJNWMra1Jy9idj-Az-iRGpuCV5-Kcn5-P_8CP0Dkl15RAdgME6DwPCmJ2hAZAeRZlMYHjX80EOUUj79ckjAgWTQbofvwqnVSdcdZ3VnncVHjetzYYlx4_f75_LOUe571rnNzgWdPhxzasydZ6b5va4ydv6xccUmrt5Bk6qeTGm9HPHaLV7WQ1nkWLh-ndOF9EisWJiJTIWApQUc2ztJKckaykhPISuOQAqSBKABhNiNKaQFpqXYpECMO1KWPFhujiENu65q03vivWTe_q8LGAJOU8FiTlgbo6UMo13jtTFa2zW-n2BSXFd2XF38oCzg74zm7M_l-2mE-XecJ5JtgXTfZsBg</recordid><startdate>202109</startdate><enddate>202109</enddate><creator>Weigt, D. M.</creator><creator>Jackman, C. M.</creator><creator>Vogt, M. F.</creator><creator>Manners, H.</creator><creator>Dunn, W. R.</creator><creator>Gladstone, G. R.</creator><creator>Kraft, R.</creator><creator>Branduardi‐Raymont, G.</creator><creator>Louis, C. K.</creator><creator>McEntee, S. C.</creator><general>Blackwell Publishing Ltd</general><scope>24P</scope><scope>WIN</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0002-6620-6357</orcidid><orcidid>https://orcid.org/0000-0002-3276-7420</orcidid><orcidid>https://orcid.org/0000-0003-0060-072X</orcidid><orcidid>https://orcid.org/0000-0003-0635-7361</orcidid><orcidid>https://orcid.org/0000-0002-0383-6917</orcidid><orcidid>https://orcid.org/0000-0001-5427-6537</orcidid><orcidid>https://orcid.org/0000-0002-9552-8822</orcidid><orcidid>https://orcid.org/0000-0003-4885-8615</orcidid></search><sort><creationdate>202109</creationdate><title>Characteristics of Jupiter's X‐Ray Auroral Hot Spot Emissions Using Chandra</title><author>Weigt, D. M. ; Jackman, C. M. ; Vogt, M. F. ; Manners, H. ; Dunn, W. R. ; Gladstone, G. R. ; Kraft, R. ; Branduardi‐Raymont, G. ; Louis, C. K. ; McEntee, S. 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M.</creatorcontrib><creatorcontrib>Jackman, C. M.</creatorcontrib><creatorcontrib>Vogt, M. F.</creatorcontrib><creatorcontrib>Manners, H.</creatorcontrib><creatorcontrib>Dunn, W. R.</creatorcontrib><creatorcontrib>Gladstone, G. R.</creatorcontrib><creatorcontrib>Kraft, R.</creatorcontrib><creatorcontrib>Branduardi‐Raymont, G.</creatorcontrib><creatorcontrib>Louis, C. K.</creatorcontrib><creatorcontrib>McEntee, S. C.</creatorcontrib><collection>Wiley Online Library Open Access</collection><collection>Wiley Online Library</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Journal of geophysical research. Space physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Weigt, D. M.</au><au>Jackman, C. M.</au><au>Vogt, M. F.</au><au>Manners, H.</au><au>Dunn, W. R.</au><au>Gladstone, G. R.</au><au>Kraft, R.</au><au>Branduardi‐Raymont, G.</au><au>Louis, C. K.</au><au>McEntee, S. C.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Characteristics of Jupiter's X‐Ray Auroral Hot Spot Emissions Using Chandra</atitle><jtitle>Journal of geophysical research. Space physics</jtitle><date>2021-09</date><risdate>2021</risdate><volume>126</volume><issue>9</issue><epage>n/a</epage><issn>2169-9380</issn><eissn>2169-9402</eissn><abstract>To help understand and determine the driver of jovian auroral X‐rays, we present the first statistical study to focus on the morphology and dynamics of the jovian northern hot spot (NHS) using Chandra data. The catalog we explore dates from December 18, 2000 up to and including September 8, 2019. Using a numerical criterion, we characterize the typical and extreme behavior of the concentrated NHS emissions across the catalog. The mean power of the NHS is found to be 1.91 GW with a maximum brightness of 2.02 Rayleighs (R), representing by far the brightest parts of the jovian X‐ray spectrum. We report a statistically significant region of emissions at the NHS center which is always present, the averaged hot spot nucleus (AHSNuc), with mean power of 0.57 GW and inferred average brightness of ∼1.2 R. We use a flux equivalence mapping model to link this distinct region of X‐ray output to a likely source location and find that the majority of mappable NHS photons emanate from the pre‐dusk to pre‐midnight sector, coincident with the dusk flank boundary. A smaller cluster maps to the noon magnetopause boundary, dominated by the AHSNuc, suggesting that there may be multiple drivers of X‐ray emissions. On application of timing analysis techniques (Rayleigh, Monte Carlo, Jackknife), we identify several instances of statistically significant quasi‐periodic oscillations (QPOs) in the NHS photons ranging from ∼2.3 to 36.4 min, suggesting possible links with ultra‐low frequency activity on the magnetopause boundary (e.g., dayside reconnection, Kelvin‐Helmholtz instabilities).
Plain Language Summary
The auroral emissions (northern and southern lights) on Jupiter are the most powerful in our Solar System and have been observed across the electromagnetic spectrum. The cause, or driver, of Jupiter's auroras is still an open question with lots of scientific debate. The solar wind can have an effect, as can Jupiter's volcanic moon Io. The plasma and magnetic field interactions can produce auroras on Jupiter in the X‐ray waveband. These powerful X‐ray emissions can be observed by telescopes like the Chandra X‐ray Observatory (CXO) that orbit Earth. The X‐ray data we analyze here have been found to flash or pulsate at certain periods, spanning the ∼20 years Chandra has observed Jupiter. We use mapping and timing analysis techniques to analyze the entire catalog from the high‐resolution camera on‐board Chandra. We report significant auroral X‐ray regions and pulsations in the North to help us provide an answer for the possible multiple X‐ray drivers.
Key Points
We present the first statistical study looking at the behavior of Jupiter's northern X‐ray auroral hot spot from 20 years of Chandra data
The X‐rays map close to the magnetopause from noon to dusk, with the center of the averaged hot spot emissions mapping to noon
Our analysis suggests that the X‐ray driver(s) may be linked with ultra‐low frequency wave activity along the magnetopause</abstract><cop>Washington</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1029/2021JA029243</doi><tpages>21</tpages><orcidid>https://orcid.org/0000-0002-6620-6357</orcidid><orcidid>https://orcid.org/0000-0002-3276-7420</orcidid><orcidid>https://orcid.org/0000-0003-0060-072X</orcidid><orcidid>https://orcid.org/0000-0003-0635-7361</orcidid><orcidid>https://orcid.org/0000-0002-0383-6917</orcidid><orcidid>https://orcid.org/0000-0001-5427-6537</orcidid><orcidid>https://orcid.org/0000-0002-9552-8822</orcidid><orcidid>https://orcid.org/0000-0003-4885-8615</orcidid><oa>free_for_read</oa></addata></record> |
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| ispartof | Journal of geophysical research. Space physics, 2021-09, Vol.126 (9), p.n/a |
| issn | 2169-9380 2169-9402 |
| language | eng |
| recordid | cdi_proquest_journals_2576648076 |
| source | Wiley-Blackwell Journals |
| subjects | aurora Auroral emissions Auroras Brightness Hot spots (geology) jovian magnetosphere Jupiter Jupiter atmosphere Magnetic fields Magnetopause magnetosphere Mapping Mean Morphology Photons Planetary magnetic fields Solar system Solar wind Solar wind effects Space telescopes Telescopes ULF waves Wind effects X‐ray aurora |
| title | Characteristics of Jupiter's X‐Ray Auroral Hot Spot Emissions Using Chandra |
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