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Interplanetary Dust Clouds near 1 AU Detected by STEREO

Interplanetary Dust Clouds near 1 AU Detected by STEREO. M. L. Kaiser, K. Goetz, C. St. Cyr, R. Howard. From Gurnett et al., Icarus , 53 , 236-254 (1983). Ecliptic longitude plot. Gr ü n’s Interplanetary Dust Distribution at 1 AU Grün, E, et al., Icarus, 62 , 244-272 (1985).

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Interplanetary Dust Clouds near 1 AU Detected by STEREO

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  1. Interplanetary Dust Clouds near 1 AU Detected by STEREO M. L. Kaiser, K. Goetz, C. St. Cyr, R. Howard

  2. From Gurnett et al., Icarus, 53, 236-254 (1983)

  3. Ecliptic longitude plot

  4. Grün’s Interplanetary Dust Distribution at 1 AU Grün, E, et al., Icarus, 62, 244-272 (1985) The BIG problem Observed flux Implied mass

  5. Coronagraphs are sensitive to faint intensities and have detected debris in the past SMM C/P [believed to be MLI] SOHO LASCO [believed to be MLI] Skylab ATM S052 [water dumps]

  6. SECCHI Debris Examples • Examples from Ahead, but also seen in Behind • Not detected in HI2-A or –B(?) • Coincident with S/WAVES impulse

  7. Summary • S/WAVES observes impulse-like signatures consistent with dust impacts • Most prominent on Ahead • Weaker and less frequent on Behind • Most prominent on antenna closest to ‘ram’ direction (X on Ahead, Z on Behind) • Most events consistent with 1-10 micron sized particles • Occurrence in ecliptic longitude consistent with known wire antenna breaks • Sharp onset at ~309° observed by Ahead, GPS/DMSP, and Behind • S/WAVES impulse signatures coincident with ‘debris’ observed by SECCHI • SECCHI debris ~20 times as prevalent as on SOHO • Limited number of events compared • Implied mass and flux during active sectors much higher than Grün distribution • In general agreement during inactive sectors

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