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SbandObservingInfo
SbandObservingInfo

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[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
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!![{TableOfContents}]
[{TableOfContents}]
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!Eclipse Season
!Eclipse Season (XTW)
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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 (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
As of 2009, JAXA ephemeris calculations for Hinode included the calculation of nominal EUV and X-ray night (known as XTW). The duration of these is approximately 30 minutes at the peak of eclipse season (2009). This is calculated from a static model, and so doesn't take into account expansion of the ionosphere with increased solar activity, which would lengthen these obscuration periods.
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At the middle of eclipse season, clear EUV day (i.e., not including transition into or out of eclipse) lasts for approximately 60 minutes (not taking into account expansion of the ionosphere with increased solar activity).
For some more information, see the notes on [EclipseEffects].
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There is often a substantial overlap between SAA and NGT events around the orbit. However, the phase of EUV night does not change phase in the orbit (whereas that of the SAA does). Therefore eclipses and SAA passes sometimes coincide (with night being the longer event), and sometimes do not overlap so much. However, there is almost always some overlap. (The exception to this is during the Golden Period, during which there are no SAA periods, but EUV nights continue to occur once per orbit).
There is often a substantial overlap between SAA and XTW (X-ray / EUV night) events around the orbit. However, the phase of EUV night does not change phase in the orbit in the way that that of the SAA does. Therefore nights and SAA passes sometimes coincide (with night being the longer event), and sometimes do not overlap so much. However, there is almost always some overlap. The exception to this is during the ''Golden Period'', during which there are no SAA events, but EUV nights continue to occur once per orbit.
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As a result, a some parts of the day, the less-than-complete overlap of SAA and night means that the clear window for observing in such orbits can be shorter. Taking into account the buffers (summarised below) around orbital events, the distribution of clear observing windows, calculated from a typical mid-eclipse season OBEV file, ranged from 58 to 68 minutes, with a modal value of 61 minutes.
As a result, at many times of day, the less-than-complete overlap of SAA and night means that the clear window for observing in such orbits can be shorter. From 2009, EUV Night event were calculated for Hinode's orbit. So taking into account the buffers (summarised below) around orbital events, we can recalculate the distribution of clear observing windows from the middle of eclipse season in 2009.
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[{Image src='attach/SbandObservingInfo/Picture%202a.png'}]
The histograms below show a distribution of these windows' length over a three-day sample. There are two distinct populations (ignore the very short windows at the far left: these are due to vanishingly small SAA events that occur shortly after larger events).
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The main population follows a distribution ranging from 44 to 62 minutes, with a mode and median of around 53 minutes in length. The second population is on the far right, and corresponds to observing windows in the Golden Period where there are no SAAs, and these windows are 65 minutes long.
The sum of all this means that if you want to be of a single raster or study fitting in between eclipses, it needs to be no more than 44 minutes long (the minimum window length). However, if you are happy accepting some curtailment of the raster at one or both ends outside the Golden Period, in order to make full use of those windows that fall inside the Golden Period, then you might design a study to have maximum 65 minutes' duration. It is a gamble, obviously, because they aren't so well suited to the majority of the observing day, and cause difficulties in forecasting the telemetry that will be accumulated because images will be taken when EIS can't see the Sun.
[{Image src='attach/SbandObservingInfo/Picture 42.png'}]
!XRT Synoptic Re-pointings
One caveat to the above information on observing windows is that (currently) twice a day, Hinode's X-Ray Telescope (''XRT'') makes a so-called synoptic observation of the Sun. This requires the satellite to point at solar disc centre. However, because XRT is sensitive to particle radiation, and X-ray nights are almost equivalent to EUV nights, it requires these observations to be taken during one of the clear observing windows (above). The duration of XRT's programme (including the time taken to re-point) is 10 minutes. Factoring in the 2 minutes post-pointing delay after the synoptic, this means that observing windows (typically, those closest to or including 06:00 and 18:00 UT) are curtailed by 12 minutes.
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| {{{NGT_ENTRY}}} | 10 minutes before
| {{{NGT_EXIT}}} | 10 minutes after
| {{{XTW_ENTRY}}} | 2 minutes before
| {{{XTW_EXIT}}} | 2 minutes after
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__Please note__ that as of late 2008, the planning tool has a "SHOW OBEV WINDOWS" feature that factors in these buffers. This feature is shown in the screenshot below
[{Image src='attach/SbandObservingInfo/OBEV%20Windows.png'}]
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Since moving to Hinode's S-band antenna for downlinks, the spacecraft typically can downlink something like 200 Mb[2] per 24 hours. This is worked out by the total contact time at all ground-stations, multiplied by the bandwidth to the ground.
Since moving to Hinode's S-band antenna for downlinks, EIS typically can downlink something like 600 Mb[2] per 24 hours. This is worked out by the total contact time at all ground-stations, in the coming OP Period, multiplied by the bandwidth to the ground[4]. Typical HOPs should be targeted to something like 250 Mb per day. __However__ , this is a rough guideline only, because the amount of telemetry that it's possible to downlink per day downlinked is quite variable, due to a number of practical factors.
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For the most recent daily allocations, you should visit the [Hinode Daily Events|http://www.isas.jaxa.jp/home/solar/hinode_op/hinode_daily_events.php] webpages, where operations are documented, and check the typical allocation for EIS over the last few weeks. (Remember to halve this number to get a rough idea of the volume you should limit yourself to).
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!!!Why can my old HOP no longer be run?
!!!How is the HOP process different?
!!!Hinode Operation Plans (HOPs)
This is the typical banner under which joint observations with Hinode are planned. HOPs are recommended by the Science Schedule Co-ordinators for [these types of observations|http://www.isas.jaxa.jp/home/solar/guidance/node5.html].
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!!ISAS site guidance
We warmly encourage you to use Hinode in achieving your scientific objectives.
The [ISAS Hinode Operations website|http://www.isas.jaxa.jp/home/solar/hinode_op/] has a link to a new section on [Guidance for Hinode Observations|http://www.isas.jaxa.jp/home/solar/guidance/guidance.html], which is worth reading through in preparation for making a proposal.
!!Why can my old HOP no longer be run?
For background on the switch from X-band to S-band telemetering of data by Hinode, take a look at the [Hinode Science Schedule Co-ordinators' announcement|http://www.isas.jaxa.jp/home/solar/guidance/node1.html], first released in SolarNews.
!!How is the HOP process different?
In short, the answer to this is: not very much :-)
Eighteen months of post-commisioning experience has given the Hinode team time to work out the kind of information and lead time that proposers and team personnel need in order to run observations successfully. So now, this information has been made available as [''Guidance for proposal observations (HOP)''|http://www.isas.jaxa.jp/home/solar/guidance/node2.html] on the ISAS Hinode website.
This page (revision-76) was last changed on 07-Dec-2016 14:14 by BriazWearlTop