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This page was created on 25-Jun-2008 06:03 by David R Williams

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!Post-pointing delay
In order to have co-ordinated observations by its three instruments, Hinode points as a whole satellite (using its AOCS[6]), either tracking a point to compensate for the (differential) rotation of the Sun, or focusing on a fixed point. Either way, movements by the s/c require the reaction wheels of the AOCS to change angular speed. After approximately 90 seconds, these speeds allow the spacecraft to track or fix on a point with better than 1" accuracy.
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To avoid observing during the stabilisation of pointing, EIS observations normally start at least two minutes after a satellite re-point.
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The duration of night-time is calculated for the visible band, and in the peak of eclipse season (around mid-July [3]) this duration is about 20 minutes. EUV absorption begins about 10 minutes before the calculated entry into optical night (NGT_ENTRY) and ends about 10 minutes after exit (NGT_EXIT). Thus, the EIS operations team recommend that you leave a ten-minute buffer around s/c night in eclipse season.
The duration of night-time is calculated for the visible band, and in the peak of eclipse season (around mid-July [3]) this duration is about 20 minutes. EUV absorption (night ingress) begins about 10 minutes before the calculated entry into optical night (listed as NGT_ENTRY) and ends (night egress) in the EUV about 10 minutes after the optical band exit (NGT_EXIT). Thus, the EIS operations team recommend that you leave a ten-minute buffer around s/c night in eclipse season where possible. Extended-duration observations
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In the middle of eclipse season, EUV day lasts for approximately
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On most orbits, Hinode passes over the South Atlantic Anomaly (SAA), where high-energy particles penetrate lower into the magnetosphere. During such passes, significantly more ''cosmic rays'' are observed on the EIS detector images. These passes are calculated at the same time as other orbital events (such as Eclipse Season NGT events, when appropriate), and times vary each day. Such passes normally last approximately 10 to 20 minutes.
On most orbits, Hinode passes over the South Atlantic Anomaly (SAA), where high-energy particles penetrate lower into the magnetosphere. During such passes, significantly more ''cosmic rays'' are observed on the EIS detector images. These passes are calculated at the same time as other orbital events (such as Eclipse Season NGT events, when appropriate), and times vary each day. Such passes normally last approximately 10 to 20 minutes (although they can be calculated to last for as little as 30 seconds).
This page (revision-76) was last changed on 07-Dec-2016 14:14 by BriazWearlTop