DMSP observations of equatorial plasma bubbles in the topside ionosphere near solar maximum

Huang, Chao‐Song; Burke, William J.; Machuzak, J. S.; Gentile, L. C.; Sultan, P. J.

doi:10.1029/2000ja000319

Cited by 173 publications

(281 citation statements)

References 36 publications

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“…The ESF studies using ionosonde data (Sales et al, 1996;Stephan et al, 2002;Whalen, 2002), the Global Positioning System (GPS) (Aarons et al, 1996;Mendillo et al, 2000Mendillo et al, , 2001, radars (Woodman and LaHoz, 1976;Hysell and Burcham, 1998), satellite (Huang et al, 2001;Su et al, 2001), and numerical modeling (Maruyama, 1988;Sultan, 1996) have demonstrated the general morphology of the ESF phenomenon. Now, it is known that there are some candidate mechanisms helping the ESF development.…”

Section: Introductionmentioning

confidence: 99%

The effects of the pre-reversal ExB drift, the EIA asymmetry, and magnetic activity on the equatorial spread F during solar maximum

et al. 2005

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Abstract. We use a digisonde at Jicamarca and a chain of GPS receivers on the west side of South America to investigate the effects of the pre-reversal enhancement (PRE) in E×B drift, the asymmetry (I a ) of equatorial ionization anomaly (EIA), and the magnetic activity (K p ) on the generation of equatorial spread F (ESF). Results show that the ESF appears frequently in summer (November, December, January, and February) and equinoctial (March, April, September, and October) months, but rarely in winter (May, June, July, and August) months. The seasonal variation in the ESF is associated with those in the PRE E×B drift and I a . The larger E×B drift (>20 m/s) and smaller |I a | (<0.3) in summer and equinoctial months provide a preferable condition to development the ESF. Conversely, the smaller E×B drift and larger |I a | are responsible for the lower ESF occurrence in winter months. Regarding the effects of magnetic activity, the ESF occurrence decreases with increasing K p in the equinoctial and winter months, but not in the summer months. Furthermore, the larger and smaller E×B drifts are presented under the quiet (K p <3) and disturbed (K p ≥3) conditions, respectively. These results indicate that the suppression in ESF and the decrease in E×B drifts are mainly caused by the decrease in the eastward electric field.

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Section: Introductionmentioning

confidence: 99%

The effects of the pre-reversal ExB drift, the EIA asymmetry, and magnetic activity on the equatorial spread F during solar maximum

et al. 2005

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“…Global maps of ESF related occurrence rates were derived from satellite observations of local plasma depletions (e.g. Kil and Heelis, 1998;Huang et al, 2001;Palmroth et al, 2001;Burke et al, 2004;Park et al, 2005) or from total electron content observations at a ground-based GPS receiver network (Nishioka et al, 2008). Alternatively, Stolle et al (2006) obtained the ESF distribution from magnetic signatures of the instabilities.…”

Section: Introductionmentioning

confidence: 99%

Relation between the occurrence rate of ESF and the equatorial vertical plasma drift velocity at sunset derived from global observations

2008

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Abstract. In this study, we investigate two global climatological data sets; the occurrence rate of Equatorial Spread-F (ESF), associated with equatorial plasma irregularities, at ∼400 km altitude obtained from CHAMP observations, and the evening equatorial vertical plasma drift, v z , from ROCSAT-1 measurements. First, as retrieved for a solar flux level of F10.7=150, the longitudinal variation of the two independently derived quantities correlates between 84% and 93% in the seasons December solstice, equinox and June solstice. The highest correlation is found for the solstice seasons when v z is integrated over local time around the prereversal enhancement (PRE) and displaced 6 • towards east. The integrated v z is a suitable estimate of the ionospheric height at the time just after the PRE and the 6 • displacement is consistent with ESF eastward drift during 2 h which is assumed between creation and detection at satellite altitudes. Second, our analyses reveal a global threshold v z which is required to observe ESF at satellite altitudes. This threshold depends linearly on solar flux with correlations of 97%. Both results bring global evidence on the linear relations between ESF and the vertical plasma drift which have been proven only by local observations so far. This paper includes the first global map of the seasonal/longitudinal variation of the ESF occurrence rate over local time being valid for high solar flux years [2001][2002][2003][2004]. The map reveals, e.g. a longitudinal dependence of the persistence of the plasma irregularities indicating that longitude dependent mechanisms other than the PRE determine the ESF lifetime.

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“…Notably, only one bubble has been observed by ROCSAT-1 in August and none during May-July (0%). Such distribution for the two-peak variation in bubble occurrence has also been proposed by Huang et al (2001) and Whalen (2002). Huang et al (2001) showed that DMSP F9 measured the highest occurrences of the equatorial plasma bubble over Huancayo (their Fig.…”

Section: Seasonal Occurrences Of Bssf and Bubble Formationmentioning

confidence: 92%

“…Whalen, 1997Whalen, , 2002Fejer et al, 1999;Huang, 2001;Su et al, 2001). The past results indicate that the occurrences of both BSSF and bubble depend on season, longitude, solar cycle, and geomagnetic activity (Maruyama and Matuura, 1984;Whalen, 1997Whalen, , 2002Fejer et al, 1999;Huang, 2001;Lee at al., 2005). Nevertheless, little work has been published examining the simultaneous occurrence of BSSF and bubble in the equatorial ionosphere (Whalen, 1997(Whalen, , 2002.…”

Section: Introductionmentioning

confidence: 99%

Concurrent study of bottomside spread F and plasma bubble events in the equatorial ionosphere during solar maximum using digisonde and ROCSAT-1

Lee

Reinisch

2005

Ann. Geophys.

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Abstract. Data from the Jicamarca digisonde and the ROCSAT-1 satellite are employed to study the equatorial ionosphere on the west side of South America during April 1999-March 2000 for the concurrent bottomside spread F (BSSF) and plasma bubble events. This study, using digisonde and ROCSAT-1 concurrently, is the first attempt to investigate the equatorial spread F. Results show that BSSF and plasma bubble observations appear frequently respectively in the summer (January, February, November, and December) and in the equinoctial (March, April, September, and October) months, respectively, but are both rarely observed in the winter (May-August) months. The upward drift velocity during the concurrent BSSF and bubble observations has been determined to study the driving mechanism. This analysis shows that large vertical drift velocities favor BSSF and bubble formations in the equinoctial and summer months. Conversely, the smaller upward velocities during the winter months cause fewer BSSF and bubble occurrences. For the geomagnetic effect, the BSSF/bubble occurrence decreases with an increasing K p value in the equinoctial months, but no such correlation is found for the summer and winter months. Moreover, the anti-correlations between K p and dh F /dt are apparent in the equinoctial months, but not in the summer and winter months. These results indicate that in the equinoctial months the BSSF/bubble generations and the pre-reversal drift velocity can be suppressed by geomagnetic activity, because the disturbance dynamo effects could have decreased the eastward electric field near sunset. However, BSSF and bubble occurrences may not be suppressed by the geomagnetic activity in the summer and winter months.

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DMSP observations of equatorial plasma bubbles in the topside ionosphere near solar maximum

Cited by 173 publications

References 36 publications

The effects of the pre-reversal ExB drift, the EIA asymmetry, and magnetic activity on the equatorial spread F during solar maximum

The effects of the pre-reversal ExB drift, the EIA asymmetry, and magnetic activity on the equatorial spread F during solar maximum

Relation between the occurrence rate of ESF and the equatorial vertical plasma drift velocity at sunset derived from global observations

Concurrent study of bottomside spread F and plasma bubble events in the equatorial ionosphere during solar maximum using digisonde and ROCSAT-1

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