Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon
Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simul...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Chané, E. [verfasserIn] |
|---|
| Format: |
E-Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2018transfer abstract |
|---|
| Schlagwörter: |
|---|
| Umfang: |
8 |
|---|
| Übergeordnetes Werk: |
Enthalten in: ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS - Mekaroonkamol, Parit ELSEVIER, 2023, Kidlington [u.a.] |
|---|---|
| Übergeordnetes Werk: |
volume:158 ; year:2018 ; day:1 ; month:09 ; pages:110-117 ; extent:8 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.pss.2018.04.023 |
|---|
| Katalog-ID: |
ELV043317952 |
|---|
| LEADER | 01000caa a22002652 4500 | ||
|---|---|---|---|
| 001 | ELV043317952 | ||
| 003 | DE-627 | ||
| 005 | 20230626003505.0 | ||
| 007 | cr uuu---uuuuu | ||
| 008 | 180726s2018 xx |||||o 00| ||eng c | ||
| 024 | 7 | |a 10.1016/j.pss.2018.04.023 |2 doi | |
| 028 | 5 | 2 | |a GBV00000000000251A.pica |
| 035 | |a (DE-627)ELV043317952 | ||
| 035 | |a (ELSEVIER)S0032-0633(17)30473-7 | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | |a 620 | |
| 082 | 0 | 4 | |a 620 |q DE-600 |
| 082 | 0 | 4 | |a 610 |q VZ |
| 084 | |a 44.87 |2 bkl | ||
| 100 | 1 | |a Chané, E. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| 264 | 1 | |c 2018transfer abstract | |
| 300 | |a 8 | ||
| 336 | |a nicht spezifiziert |b zzz |2 rdacontent | ||
| 337 | |a nicht spezifiziert |b z |2 rdamedia | ||
| 338 | |a nicht spezifiziert |b zu |2 rdacarrier | ||
| 520 | |a Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). | ||
| 520 | |a Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). | ||
| 650 | 7 | |a Jupiter |2 Elsevier | |
| 650 | 7 | |a Magnetosphere |2 Elsevier | |
| 650 | 7 | |a Solar wind |2 Elsevier | |
| 700 | 1 | |a Palmaerts, B. |4 oth | |
| 700 | 1 | |a Radioti, A. |4 oth | |
| 773 | 0 | 8 | |i Enthalten in |n Elsevier Science |a Mekaroonkamol, Parit ELSEVIER |t ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |d 2023 |g Kidlington [u.a.] |w (DE-627)ELV010254102 |
| 773 | 1 | 8 | |g volume:158 |g year:2018 |g day:1 |g month:09 |g pages:110-117 |g extent:8 |
| 856 | 4 | 0 | |u https://doi.org/10.1016/j.pss.2018.04.023 |3 Volltext |
| 912 | |a GBV_USEFLAG_U | ||
| 912 | |a GBV_ELV | ||
| 912 | |a SYSFLAG_U | ||
| 912 | |a SSG-OLC-PHA | ||
| 912 | |a GBV_ILN_66 | ||
| 912 | |a GBV_ILN_91 | ||
| 912 | |a GBV_ILN_165 | ||
| 912 | |a GBV_ILN_234 | ||
| 936 | b | k | |a 44.87 |j Gastroenterologie |q VZ |
| 951 | |a AR | ||
| 952 | |d 158 |j 2018 |b 1 |c 0901 |h 110-117 |g 8 | ||
| 953 | |2 045F |a 620 | ||
| author_variant |
e c ec |
|---|---|
| matchkey_str |
chanepalmaertsbradiotia:2018----:eidchaigoiniteoinantshrcuiglclzdeknhm |
| hierarchy_sort_str |
2018transfer abstract |
| bklnumber |
44.87 |
| publishDate |
2018 |
| allfields |
10.1016/j.pss.2018.04.023 doi GBV00000000000251A.pica (DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Chané, E. verfasserin aut Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon 2018transfer abstract 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier Palmaerts, B. oth Radioti, A. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 https://doi.org/10.1016/j.pss.2018.04.023 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 158 2018 1 0901 110-117 8 045F 620 |
| spelling |
10.1016/j.pss.2018.04.023 doi GBV00000000000251A.pica (DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Chané, E. verfasserin aut Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon 2018transfer abstract 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier Palmaerts, B. oth Radioti, A. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 https://doi.org/10.1016/j.pss.2018.04.023 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 158 2018 1 0901 110-117 8 045F 620 |
| allfields_unstemmed |
10.1016/j.pss.2018.04.023 doi GBV00000000000251A.pica (DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Chané, E. verfasserin aut Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon 2018transfer abstract 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier Palmaerts, B. oth Radioti, A. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 https://doi.org/10.1016/j.pss.2018.04.023 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 158 2018 1 0901 110-117 8 045F 620 |
| allfieldsGer |
10.1016/j.pss.2018.04.023 doi GBV00000000000251A.pica (DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Chané, E. verfasserin aut Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon 2018transfer abstract 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier Palmaerts, B. oth Radioti, A. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 https://doi.org/10.1016/j.pss.2018.04.023 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 158 2018 1 0901 110-117 8 045F 620 |
| allfieldsSound |
10.1016/j.pss.2018.04.023 doi GBV00000000000251A.pica (DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 DE-627 ger DE-627 rakwb eng 620 620 DE-600 610 VZ 44.87 bkl Chané, E. verfasserin aut Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon 2018transfer abstract 8 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier Palmaerts, B. oth Radioti, A. oth Enthalten in Elsevier Science Mekaroonkamol, Parit ELSEVIER ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS 2023 Kidlington [u.a.] (DE-627)ELV010254102 volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 https://doi.org/10.1016/j.pss.2018.04.023 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 44.87 Gastroenterologie VZ AR 158 2018 1 0901 110-117 8 045F 620 |
| language |
English |
| source |
Enthalten in ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS Kidlington [u.a.] volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 |
| sourceStr |
Enthalten in ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS Kidlington [u.a.] volume:158 year:2018 day:1 month:09 pages:110-117 extent:8 |
| format_phy_str_mv |
Article |
| bklname |
Gastroenterologie |
| institution |
findex.gbv.de |
| topic_facet |
Jupiter Magnetosphere Solar wind |
| dewey-raw |
620 |
| isfreeaccess_bool |
false |
| container_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| authorswithroles_txt_mv |
Chané, E. @@aut@@ Palmaerts, B. @@oth@@ Radioti, A. @@oth@@ |
| publishDateDaySort_date |
2018-01-01T00:00:00Z |
| hierarchy_top_id |
ELV010254102 |
| dewey-sort |
3620 |
| id |
ELV043317952 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV043317952</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230626003505.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180726s2018 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.pss.2018.04.023</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000251A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV043317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0032-0633(17)30473-7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">620</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">610</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">44.87</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Chané, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">8</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014).</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014).</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Jupiter</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Magnetosphere</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Solar wind</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Palmaerts, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Radioti, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="n">Elsevier Science</subfield><subfield code="a">Mekaroonkamol, Parit ELSEVIER</subfield><subfield code="t">ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS</subfield><subfield code="d">2023</subfield><subfield code="g">Kidlington [u.a.]</subfield><subfield code="w">(DE-627)ELV010254102</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:158</subfield><subfield code="g">year:2018</subfield><subfield code="g">day:1</subfield><subfield code="g">month:09</subfield><subfield code="g">pages:110-117</subfield><subfield code="g">extent:8</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1016/j.pss.2018.04.023</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ELV</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHA</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_66</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_91</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_165</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_234</subfield></datafield><datafield tag="936" ind1="b" ind2="k"><subfield code="a">44.87</subfield><subfield code="j">Gastroenterologie</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">158</subfield><subfield code="j">2018</subfield><subfield code="b">1</subfield><subfield code="c">0901</subfield><subfield code="h">110-117</subfield><subfield code="g">8</subfield></datafield><datafield tag="953" ind1=" " ind2=" "><subfield code="2">045F</subfield><subfield code="a">620</subfield></datafield></record></collection>
|
| author |
Chané, E. |
| spellingShingle |
Chané, E. ddc 620 ddc 610 bkl 44.87 Elsevier Jupiter Elsevier Magnetosphere Elsevier Solar wind Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| authorStr |
Chané, E. |
| ppnlink_with_tag_str_mv |
@@773@@(DE-627)ELV010254102 |
| format |
electronic Article |
| dewey-ones |
620 - Engineering & allied operations 610 - Medicine & health |
| delete_txt_mv |
keep |
| author_role |
aut |
| collection |
elsevier |
| remote_str |
true |
| illustrated |
Not Illustrated |
| topic_title |
620 620 DE-600 610 VZ 44.87 bkl Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon Jupiter Elsevier Magnetosphere Elsevier Solar wind Elsevier |
| topic |
ddc 620 ddc 610 bkl 44.87 Elsevier Jupiter Elsevier Magnetosphere Elsevier Solar wind |
| topic_unstemmed |
ddc 620 ddc 610 bkl 44.87 Elsevier Jupiter Elsevier Magnetosphere Elsevier Solar wind |
| topic_browse |
ddc 620 ddc 610 bkl 44.87 Elsevier Jupiter Elsevier Magnetosphere Elsevier Solar wind |
| format_facet |
Elektronische Aufsätze Aufsätze Elektronische Ressource |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
zu |
| author2_variant |
b p bp a r ar |
| hierarchy_parent_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| hierarchy_parent_id |
ELV010254102 |
| dewey-tens |
620 - Engineering 610 - Medicine & health |
| hierarchy_top_title |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| isfreeaccess_txt |
false |
| familylinks_str_mv |
(DE-627)ELV010254102 |
| title |
Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| ctrlnum |
(DE-627)ELV043317952 (ELSEVIER)S0032-0633(17)30473-7 |
| title_full |
Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| author_sort |
Chané, E. |
| journal |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| journalStr |
ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
600 - Technology |
| recordtype |
marc |
| publishDateSort |
2018 |
| contenttype_str_mv |
zzz |
| container_start_page |
110 |
| author_browse |
Chané, E. |
| container_volume |
158 |
| physical |
8 |
| class |
620 620 DE-600 610 VZ 44.87 bkl |
| format_se |
Elektronische Aufsätze |
| author-letter |
Chané, E. |
| doi_str_mv |
10.1016/j.pss.2018.04.023 |
| dewey-full |
620 610 |
| title_sort |
periodic shearing motions in the jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| title_auth |
Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| abstract |
Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). |
| abstractGer |
Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). |
| abstract_unstemmed |
Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014). |
| collection_details |
GBV_USEFLAG_U GBV_ELV SYSFLAG_U SSG-OLC-PHA GBV_ILN_66 GBV_ILN_91 GBV_ILN_165 GBV_ILN_234 |
| title_short |
Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon |
| url |
https://doi.org/10.1016/j.pss.2018.04.023 |
| remote_bool |
true |
| author2 |
Palmaerts, B. Radioti, A. |
| author2Str |
Palmaerts, B. Radioti, A. |
| ppnlink |
ELV010254102 |
| mediatype_str_mv |
z |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| author2_role |
oth oth |
| doi_str |
10.1016/j.pss.2018.04.023 |
| up_date |
2024-07-06T18:30:28.129Z |
| _version_ |
1803855465680994304 |
| fullrecord_marcxml |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV043317952</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230626003505.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180726s2018 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.pss.2018.04.023</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBV00000000000251A.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV043317952</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0032-0633(17)30473-7</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">620</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">610</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">44.87</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Chané, E.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Periodic shearing motions in the Jovian magnetosphere causing a localized peak in the main auroral emission close to noon</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">8</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014).</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Recently, a transient localized brightness enhancement has been observed in Jupiter's main auroral emission close to noon by Palmaerts et al. (2014). We use results from three-dimensional global MHD simulations to understand what is causing this localized peak in the main emission. In the simulations, the peak occurs every rotation period and is due to shearing motions in the magnetodisk. These shearing motions are caused by heavy flux-tubes being accelerated to large azimuthal speeds at dawn. The centrifugal force acting on these flux-tubes is then so high that they rapidly move away from the planet. When they reach noon, their azimuthal velocity decreases, thus reducing the centrifugal force, and allowing the flux-tubes to move back closer to Jupiter. The shearing motions associated with this periodic phenomenon locally increase the field aligned currents in the simulations, thus causing a transient brightness enhancement in the main auroral emission, similar to the one observed by Palmaerts et al. (2014).</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Jupiter</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Magnetosphere</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="650" ind1=" " ind2="7"><subfield code="a">Solar wind</subfield><subfield code="2">Elsevier</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Palmaerts, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Radioti, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="n">Elsevier Science</subfield><subfield code="a">Mekaroonkamol, Parit ELSEVIER</subfield><subfield code="t">ENDOLOOP-ASSISTED TRANSORAL OUTLET REDUCTION: A PILOT CASE-CONTROL STUDY OF A NEW THERAPEUTIC INTERVENTION FOR WEIGHT REGAIN AFTER ROUX-EN-Y GASTRIC BYPASS</subfield><subfield code="d">2023</subfield><subfield code="g">Kidlington [u.a.]</subfield><subfield code="w">(DE-627)ELV010254102</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:158</subfield><subfield code="g">year:2018</subfield><subfield code="g">day:1</subfield><subfield code="g">month:09</subfield><subfield code="g">pages:110-117</subfield><subfield code="g">extent:8</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield code="u">https://doi.org/10.1016/j.pss.2018.04.023</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ELV</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_U</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHA</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_66</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_91</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_165</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_234</subfield></datafield><datafield tag="936" ind1="b" ind2="k"><subfield code="a">44.87</subfield><subfield code="j">Gastroenterologie</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">158</subfield><subfield code="j">2018</subfield><subfield code="b">1</subfield><subfield code="c">0901</subfield><subfield code="h">110-117</subfield><subfield code="g">8</subfield></datafield><datafield tag="953" ind1=" " ind2=" "><subfield code="2">045F</subfield><subfield code="a">620</subfield></datafield></record></collection>
|
| score |
7.399805 |