Space & Astronomy/Space and Astronomy (October 1993).iso/mac/TEXT/SPACEDIG/V13_4/V13_469.TXT

Internet Message Format | 1991-06-28 | 26KB

Return-path: <[e-mail]>
X-Andrew-Authenticated-as: 7997;andrew.cmu.edu;Ted Anderson
Received: from hogtown.andrew.cmu.edu via trymail for +dist+/afs/andrew.cmu.edu/usr11/tm2b/space/[e-mail] (->+dist+/afs/andrew.cmu.edu/usr11/tm2b/space/space.dl) (->ota+space.digests)
          ID </afs/andrew.cmu.edu/usr1/ota/Mailbox/Uc6Evmi00WBw86dU4P>;
          Sat, 27 Apr 91 01:41:08 -0400 (EDT)
Message-ID: <[e-mail]>
Precedence: junk
Reply-To: [e-mail]
From: [e-mail]
To: [e-mail]
Date: Sat, 27 Apr 91 01:40:59 -0400 (EDT)
Subject: SPACE Digest V13 #469

SPACE Digest                                     Volume 13 : Issue 469

Today's Topics:
               Re: Saturn V and the ALS
         Re: Dan Quayle on Mars (was: "Face" on Mars)
    Magellan scientists study surface of Venus (Forwarded)
             Re: NASA & Executive Branch
         Re: "Bussard Ramjets" AKA duct space drives
        MONTHLY SOLAR TERRESTRIAL REVIEW - MARCH 1991

Administrivia:

    Submissions to the SPACE Digest/sci.space should be mailed to
  [e-mail].  Other mail, esp. [un]subscription requests,
  should be sent to [e-mail], or, if urgent, to
             [e-mail]

----------------------------------------------------------------------

Date: 26 Apr 91 18:52:02 GMT
From: agate!bionet!uwm.edu!zaphod.mps.ohio-state.edu!samsung!news.cs.indiana.edu!noose.ecn.purdue.edu!en.ecn.purdue.edu![e-mail]  (/dev/null)
Subject: Re: Saturn V and the ALS

In article <[e-mail]>, [e-mail] (Henry Spencer) writes:
> >BUT, engines could be made that burn less fuel and therefore lift
> >even more to orbit.  Maybe rocketdyne could modify the F-1 to
> >bring it up to date.
>
> Why bother?  It works fine as it is.  Fuel costs are a negligible fraction
> of launch costs, and the Saturn V's payload to orbit is adequate for most
> any foreseeable project.

The engines do NOT work fine if they help contribute to $1500+/lb to
orbit (optimistic estimate).  I suggested lowering the amount of fuel
NOT because kerosene is expensive (it's not), but to open up
more VOLUME and LIFT for payload, thus dropping costs!
the payload SIZE is wonderful (though it could be better :) ),
 its COST is terrible.  We need to get
cost per pound down below $1000/lb (preferably $200/lb).

>
> If you insist on "improving" half the subystems, *then*, yes, reviving the
> Saturn V will be extremely expensive.  The way to do it cheaply is to
> firmly refuse to redevelop anything unnecessarily.

You missed my whole point.  The Saturn V is too expensive as it iS!
We neeD launcher that gives us a large payload AND cost less than $1000/lb or
there will never be a use for it or any other "heavy launcher!"

--
+-----------------------------------------------------------------------+
| Brent L. Irvine     |            These are MY opinions   |
| Malt Beverage Analyst     |            As if they counted...:) |
+-----------------------------------------------------------------------+

------------------------------

Date: 26 Apr 91 18:37:07 GMT
From: pyramid![e-mail]  (Lon Stowell)
Subject: Re: Dan Quayle on Mars (was: "Face" on Mars)

In article <[e-mail]> [e-mail] (S Schaper) writes:
>I believe that the evidence is that Quayle is actually quite intelligent, the
>respected senator, and all that. He had a good reputation. When he hit the
>national scene, the Politically Correct crowd, hating his views, concocted
>this whole image for him, which he does help out with his gaffes and slips of
>the tongue.



But the face on Mars looks more like Margaret Thatcher than Dan
Quayle... >:-)

------------------------------

Date: 26 Apr 91 09:06:57 GMT
From: [e-mail]  (Peter E. Yee)
Subject: Magellan scientists study surface of Venus (Forwarded)

Paula Cleggett-Haleim
Headquarters, Washington, D.C.                     April 26, 1991
(Phone:  [phone])

Jim Doyle
Jet Propulstion Laboratory, Pasadena, Calif.
(Phone:  [phone])


RELEASE:  91-63

MAGELLAN SCIENTISTS STUDY SURFACE OF VENUS

    Magellan scientists at NASA's Jet Propulsion Laboratory
(JPL), Pasadena, Calif., are studying the surface features on
Venus caused by wind in the planet's dense atmosphere, Project
Scientist Steve Saunders said today.

    The movement of dust and sand is an important geological
process on planets with atmospheres, he said.  The surface
pressure of Venus' atmosphere is 90 times that of Earth's.

    Soviet landers and the U.S. Pioneer probes measured wind
speeds near the surface of Venus at  2 to 4 miles per hour (1 to
2 meters per second).  Based on theory and laboratory
experiments, that wind speed is very close to the speed required
to move sand grains on Venus, Saunders said.  Accumulations of
blown sand and dust can blanket large regions and produce visible
patterns in the Magellan radar images, he stated.

    "The most prominent wind features in the Magellan images of
Venus are wind streaks," Saunders said.  "Streaks form in the lee
of topographic obstacles by the deposition or removal of sand and
dust and can be used as indicators of the direction of the most
intense winds," he stated.

    Many large impact craters on Venus have nearby wind streaks
that may have been caused by the violent winds generated during
the impact event or that may be the result of a slower process of
subsequent wind movement of the fine impact debris.

    Magellan has mapped more than 78 percent of the planet and
by the time the primary mission cycle ends May 15, will have
mapped about 84 percent, project officials said.

    Project Manager Tony Spear said a newly adopted strategy to
protect the spacecraft from the heat of direct sunlight has been
successful in cooling the spacecraft.  Magellan has been growing
warmer as a result of changes in the geometry of Venus, Earth and
the sun and the time the spacecraft spends broadside to the sun.
A strategy, called "two-hide" which results in slightly shorter
imaging swaths, protects the spacecraft by hiding it behind the
large antenna and by turning the solar panels away for periods of
time to reduce reflection.  The  Magellan project is managed by
JPL for the Office of Space Science and Applications.

- end -

    Two photographs, one showing wind streaks near the crater
Mead and the other depicting an area of lava flow on Venus, are
available from NASA's Audio Visual Branch at 202/453-8373.

------------------------------

Date: 26 Apr 91 13:19:45 GMT
From: abvax!iccgcc![e-mail]
Subject: Re: NASA & Executive Branch

In article <[e-mail]>, [e-mail] (Bob Pendleton) writes:
>
> Oh sure they talked about checks and balances, but never about the
> mechanisms for enforcing the checks and balances. I doubt I ever had a
> teacher who understood how it worked.

Yes, the final check is the jury of twelve.
>
>> If Henry has to start telling posters how our government works, then we are
>> in big trouble.   I'm sure few of us can tell him how his works!
>
> We are already in big trouble. US public grade and secondary schools
> don't teach. Few of the teacher can teach and the ones that can teach
> aren't allowed to.
>
> How does this relate to sci.space? If you want the US to be a presence
> in space, we'd better fix our %#@&ing schools.
>
Fixing the public school system is a slow painful process, if it is
possible at all.  My children, and your children are an urgent issue.
Get them out of the public school system into an educational system
that works.  NOW!

dan herrick
[e-mail]

------------------------------

Date: 26 Apr 91 14:52:55 GMT
From: agate!usenet.ins.cwru.edu!abvax!iccgcc![e-mail]
Subject: Re: "Bussard Ramjets" AKA duct space drives

In article <[e-mail]>, [e-mail] (John A. Weeks III) writes:
>
> You better hope that you either have a uniform distribution of hydrogen,
> or you have some way to predict the density.  Consider what would happen
> if the hydrogen density suddenly increased and your engine was not expecting
> it.  You would end up with either a power surge or a "major malfunction".
>
That's an interesting question.  Here is a naive response in hope
that someone better informed will set me straight:

Isn't it reasonable to expect that hydrogen density variations in space
will be comparable to the density variations we experience in the
tellurian atmosphere?  One or two very bumpy airplane rides suggest
there are drastic variations in mass flow input to production jet
engines.

dan herrick
[e-mail]

------------------------------

Date: Fri, 26 Apr 91 20:00:26 MDT
From: oler <@BITNET.CC.CMU.EDU:[e-mail]> (CARY OLER)
Subject: MONTHLY SOLAR TERRESTRIAL REVIEW - MARCH 1991
X-St-Vmsmail-To: st%"[e-mail]"

                   ---  MONTHLY SOLAR TERRESTRIAL REVIEW  ---
                                 March 1991

                Report Issued In-Part from Data Released by the
                       Space Environment Services Center
                               Boulder Colorado

                                   --------


MONTHLY ACTIVITY SUMMARY AND SOLAR CYCLE OUTLOOK MAY 1991 - OCTOBER 1991

     We are now in month 55 of solar cycle 22.  Solar activity skyrocketed in
March, corresponding to the predicted pulse of activity which was expected
for this period late in 1990.  There were 123 energetic events in March, the
largest number of events in any calendar month this solar cycle.  There were
35 major flares, 20 of which attained class X ratings (the most powerful
x-ray classification given to solar flares).  Regions 6538, 6545 and 6555
were the major producers of flare activity this month.  Despite the high
number of solar flares which occurred in March, solar indices dropped
compared with February's values.  This drop contributes further emphasis to
the belief that July 1989 was indeed the maximum of this solar cycle as far
as sunspot numbers are concerned.

     There were a number of major events during the first half of the month,
including an optically uncorrelated long-duration class X7 event on 04 March
at 14:03 UT and an X5/3B at 07:55 UT on 07 March.  The highlights of the
month, however, began on 22 March with an X9/3B flare at 22:47 UT from Region
6555.  Large radio bursts across the spectrum and a strong Type II radio
sweep were associated with this flare.  The X9 was followed about four hours
later by an M6/2B from the same region, which lasted for nearly three and a
half hours.  These two flares are believed responsible for what is arguably
the largest proton event at greater than 10 MeV of this solar cycle.  A peak
of 43,000 p.f.u. (particle flux units) at greater than 10 MeV occurred at
03:50 UT on 24 March; the greater than 100 MeV proton flux briefly reached
100 p.f.u. at the same time.  This time also marked the passage of a powerful
interplanetary shockwave believed to have been spawned by the X9 flare.  A
magnetic SSC (Sudden Storm Commencement) measuring 184 gammas at Boulder
occurred at 03:42 UT on 24 March (more northern middle latitudes also
reported an SSC of around 180 gammas at this time - as did the southern parts
of the southern hemisphere).

     Geomagnetic conditions were at severe to minor storm levels at all
latitudes from the SSC through 26 March.  A second shock, most likely related
to the long-duration M6 flare, was observed at about 19:20 UT on 24 March.
At that time, the GOES 6 satellite began repeated crossings of the
magnetopause into the solar wind.  By about 20:00 UT, the magnetopause was
compressed well within the GOES geosynchronous orbit, and remained there
until approximately 22:10 UT on 24 March.

     This geomagnetic storm was the second largest of this solar cycle,
exceeded only by the major storm of March 13-14, 1989.  In comparison, the
planetary magnetic A-index for this most recent major storm was 115, while
the planetary magnetic A-index for the March 1989 storm 246.  The March 1989
storm was therefore a quite a bit more powerful than this most recent storm.
This storm was associated with intense auroral activity that was viewed well
into the low latitude regions.  Reports of auroral activity from northern
Texas to Georgia and South Carolina were received during this period.

     Among the other effects of this activity was a Polar Cap Absorption
(PCA) event of more than 20 dB at 02:55 UT on 24 March, a Forbush decrease
of greater than 10 percent seen on the Thule neutron monitor, and
geomagnetically induced currents (GIC) observed throughout much of Canada
and the northeastern U.S.. Reports of electrical power transformer damage
has also been reported in the northeastern U.S. during this period.

     Radio propagation conditions were severely disturbed during the major
geomagnetic storm of last March.  The combined effects of the PCA and
ionospheric storming produced the most intense widespread HF blackout
conditions observed since the major storm of March 1989.  Polar and high
latitude regions experienced continuous radio blackout conditions for days
while the middle latitude regions experienced frequent blackout to near
blackout conditions.

     Some of the best auroral backscatter communications observed on the VHF
bands since the major storm of March 1989 were observed during this recent
storm.  Widespread auroral backscatter was reported around the world, in both
the northern and southern hemispheres on 24-26 March.  VHF auroral
backscatter communications were possible into the low latitude regions during
this period.


SIX MONTH SOLAR CYCLE OUTLOOK

     This pulse of solar activity which was observed from January to March of
this year represents the predicted pulse of activity which was anticipated
late last year.  There was a concern that the activity would persist and
perhaps peak in April, but it has become apparent that the pulse of activity
peaked in March and began to diminish in April.

     Solar activity is expected to decline to more moderate levels over the
summer months.  Major flaring will occassionally be observed, but the
frequency of major flaring is expected to drop substantially over what was
observed during March.  The average solar flux and sunspot numbers are
expected to drop over the summer as we begin a slow decline back towards a
minimum in solar activity expected sometime in 1996.  However, expect many
more periods of high solar activity throughout this year and into next year.

     Geomagnetic activity between November 1990 and late February 1991 was
more stable and quiet than has been observed in over two years.  Similar
conditions are expected over the summer months.  Generally quiet to unsettled
geomagnetic activity is expected.  However, there is a risk for periods of
geomagnetic storming due to transient solar activity and recurrent coronal
activity.  A slight risk exists for another major geomagnetic and auroral
storm over the summer months due primarily to transient solar activity,
although models are less confident about this than they were about the
occurrence of a major storm with the last pulse of activity which occurred in
March.

     Over the next six months, auroral activity is expected to remain about
as active as it has been since late last year.  Although a slight risk does
exist for another major auroral storm over the summer months (as was
mentioned above), confidence levels are not as high as they were for the
March event.

     HF radio propagation conditions are expected to benefit from increased
ionospheric stability during the summer months, thereby presenting more
stable conditions for DX during these months.  However, predicted reduced
solar indices are expected to decrease the daily MUFs over all areas.  The
predicted reduction in MUFs may cause the frequency of 6 meter openings to
decline as well.  The seasonal increase in static and noise over the summer
months will also play a factor in HF propagation conditions.

     VHF propagation conditions are expected to remain generally normal
throughout the summer.  No significant periods of DX are expected, except
during local periods of favorable sporadic E.  The frequency of possible
sudden ionospheric enhancements (SIDs) is expected to decline over the
summer, although a risk does exist for periods of SID enhancements due to
transient solar activity.  The frequency of auroral backscatter
communications is not expected to change signficantly over the high latitude
and northerly middle latitude regions.  The potential for auroral
backscatter communications should remain nearly constant throughout the
summer for these areas.  For the lower latitudes, the probability for
experiecing auroral backscatter communications is reduced.


    RECENT SOLAR INDICES (PRELIMINARY) OF THE OBSERVED MONTHLY MEAN VALUES
                          Updated for March, 1991

              Sunspot Numbers                   Radio Flux    Geomagnetic
      ------------------------------------     -------------  -----------
       Observed     Ratio    Smooth Values    Ottawa  Smooth       Smooth
      SESC    RI   RI/SESC    SESC    RI       10 cm  Value    Ap  Value
      ------------------------------------     -------------  -----------
                                  YEAR = 1989
Jan:  203.2  161.6  .80       189.2  141.9     235.4  190.2    19   16.7
Feb:  211.0  164.5  .78       196.0  144.7     222.4  194.0    15   17.0
Mar:  176.8  131.0  .74       204.1  149.4     205.1  199.7    41   17.6

Apr:  172.3  129.3  .75       209.9  153.1     189.6  204.4    23   18.2
May:  207.0  138.4  .67       216.4  156.5     190.1  209.3    16   18.8
Jun:  297.3  196.0  .66       220.1  157.9     239.6  213.1    17   19.2

Jul:  193.9  126.8  .65       221.1  158.1     181.9  212.6     8   19.1
Aug:  243.0  166.8  .69       221.5  157.4     217.1  209.7    20   19.3
Sep:  240.7  176.8  .74       221.3  156.3     225.9  207.2    17   18.8

Oct:  217.4  158.5  .73       223.2  157.1     208.7  206.3    21   18.3
Nov:  255.0  173.0  .68       223.4  157.3     235.1  206.1    19   18.4
Dec:  217.8  166.1  .76       217.3  153.3     213.0  203.3    16   18.4

                                  YEAR = 1990
Jan:  239.3  179.4  .75       212.4  150.3     210.1  200.4    14   18.6
Feb:  184.7  128.4  .71       213.9  152.5     178.3  200.5    23   18.8
Mar:  198.6  140.8  .71       212.7  151.7     188.8  198.7    23   18.6

Apr:  196.1  139.8  .71       210.5  149.0     185.3  195.6    27   18.3
May:  187.7  132.0  .70       208.1  146.7     189.7  192.4    16   17.6
Jun:  168.9  105.2  .62       205.3  143.4     170.9  189.9    16   16.8

Jul:  204.3  147.0  .72       203.8  140.0     180.7  190.3    14   16.2
Aug:  269.4  199.9  .74       206.3  139.9     222.6  193.7    19   15.3
Sep:  186.4  124.7  .67       211.1  141.5*    177.4  198.1*   14   14.8*

Oct:  219.0  145.2  .66                        182.0           15
Nov:  196.1  130.5  .67                        184.3            9
Dec:  208.0  128.5  .62                        204.9            7

                                  YEAR = 1991
Jan:  213.5  136.9  .64                        228.0            8
Feb:  270.2  167.5  .62                        242.0            9
Mar:  227.9  140.6* .62*                       228.9*          23*

* = Preliminary estimates

The lowest smoothed sunspot number for Cycle 21, RI = 12.3, occurred in
September 1986.  The preliminary sunspot maximum for this cycle (cycle 22)
remains July 1989, with a peak smoothed sunspot number of 158.1.


DAILY SOLAR DATA FOR MARCH, 1991.

                         GENERAL DAILY SOLAR STATISTICS
 _____________________________________________________________________________
|       | Radio Flux  |           |  Sunspot   |           Flares             |
|       |   Ottawa    |  Sunspot  |    Area    |   X-Ray          Optical     |
|Date   |  10.7 cm    |  Number   | mil.sq.km. | C   M   X  |  S   1   2   3  |
|-------|-------------|-----------|------------|--- --- --- | --- --- --- --- |
|01 Mar |     218     |    203    |   6,030    | 9   1   0  |  7   0   1   0  |
|02 Mar |     211     |    210    |   5,760    | 7   2   0  | 11   4   0   0  |
|03 Mar |     211     |    136    |   2,400    | 3   3   0  |  6   1   0   0  |
|04 Mar |     233     |    130    |   1,680    | 2   6   1  |  2   1   1   0  |
|05 Mar |     213     |    146    |   2,490    | 4   4   3  | 11   0   2   2  |
|06 Mar |     209     |    153    |   3,720    | 9   4   0  | 11   3   0   0  |
|07 Mar |     213     |    188    |   3,840    | 7   9   2  | 22   4   1   1  |
|08 Mar |     214     |    211    |   3,660    | 6   3   1  | 15   3   1   0  |
|09 Mar |     217     |    263    |   3,690    | 1   4   0  | 12   1   1   0  |
|10 Mar |     225     |    248    |   4,920    |12   0   0  | 12   3   0   0  |
|11 Mar |     223     |    226    |   4,620    |14   1   0  | 14   2   0   0  |
|12 Mar |     231     |    248    |   5,940    |13   0   1  | 16   0   2   0  |
|13 Mar |     241     |    231    |   5,070    | 9   2   2  |  8   2   3   0  |
|14 Mar |     244     |    261    |   4,230    |14   1   1  | 22   2   0   0  |
|15 Mar |     244     |    288    |   5,130    |12   4   0  | 24   5   0   0  |
|16 Mar |     257     |    343    |   5,580    | 7   4   1  | 22   2   2   0  |
|17 Mar |     250     |    283    |   5,280    |13   7   1  | 28   7   3   0  |
|18 Mar |     276     |    267    |   6,300    | 4   6   0  | 33   8   1   0  |
|19 Mar |     262     |    230    |   6,600    | 5   4   0  |  7   2   2   0  |
|20 Mar |     250     |    264    |   9,150    |13   6   0  |  9   9   0   0  |
|21 Mar |     252     |    227    |   7,980    |11   7   1  | 15   7   3   0  |
|22 Mar |     258     |    269    |   9,390    |10   4   1  | 26   7   0   1  |
|23 Mar |     233     |    274    |   8,280    | 6   8   0  | 18   5   3   1  |
|24 Mar |     260     |    281    |   9,120    | 6   5   0  | 27   3   2   1  |
|25 Mar |     237     |    251    |   8,970    |11   1   2  | 18   4   0   2  |
|26 Mar |     230     |    248    |   8,520    |11   1   1  | 13   4   0   1  |
|27 Mar |     204     |    218    |   7,680    | 6   1   0  | 11   1   0   0  |
|28 Mar |     199     |    188    |   7,800    | 5   0   0  |  6   0   0   0  |
|29 Mar |     191     |    184    |   6,900    | 5   1   1  | 16   1   0   1  |
|30 Mar |     199     |    217    |   7,320    | 4   1   0  | 10   2   0   0  |
|31 Mar |     192     |    178    |   5,730    | 5   3   1  | 13   0   2   0  |
 -----------------------------------------------------------------------------


DAILY PLANETARY GEOMAGNETIC ACTIVITY AND PROTON FLUENCE VALUES FOR MARCH 1991

 ____________________________________________________________________________
|  Date   | Ap  | Planetary K-index | >10 MeV | >100 MeV |      Notes        |
|---------|-----|-------------------|---------|----------|-------------------|
|01 March |  13 |  2-2-2-3-3-3-3-3  | 1.7 E+4 |  3.0 E+3 |                   |
|02 March |  10 |  3-2-1-2-3-3-2-2  | 1.7 E+4 |  3.3 E+3 |                   |
|03 March |   7 |  2-1-2-2-2-2-2-2  | 2.1 E+4 |  3.1 E+3 |                   |
|04 March |   8 |  1-1-1-1-2-2-3-2  | 3.7 E+4 |  2.8 E+3 |                   |
|05 March |  23 |  2-3-5-4-4-4-3-3  | 3.5 E+4 |  2.2 E+3 |                   |
|06 March |  23 |  2-4-3-4-3-4-4-4  | 2.8 E+4 |  2.2 E+3 |                   |
|07 March |  26 |  3-4-4-4-4-3-4-4  | 1.6 E+4 |  2.8 E+3 |                   |
|08 March |  17 |  3-4-4-4-4-3-4-4  | 1.4 E+4 |  2.5 E+3 |                   |
|09 March |  24 |  4-4-3-4-4-4-3-4  | 1.7 E+4 |  2.6 E+3 | SI 33 nT = 2246UT |
|10 March |  20 |  5-5-3-4-3-2-2-1  | 1.8 E+4 |  2.2 E+3 |                   |
|11 March |   7 |  1-1-2-2-2-2-2-2  | 1.6 E+4 |  2.2 E+3 |                   |
|12 March |  16 |  2-2-3-3-3-3-4-4  | 4.7 E+4 |  2.2 E+3 | Pro. Enh.= 1800UT |
|13 March |  24 |  6-3-4-2-2-4-2-1  | 4.7 E+5 |  2.2 E+3 |                   |
|14 March |   9 |  2-2-2-3-2-1-2-1  | 3.6 E+5 |  1.7 E+3 |                   |
|15 March |   8 |  2-1-1-2-3-3-2-1  | 1.3 E+5 |  1.5 E+3 |                   |
|16 March |   9 |  1-1-1-2-2-3-4-2  | 7.3 E+4 |  1.5 E+3 |                   |
|17 March |  12 |  2-4-2-3-3-3-3-3  | 6.7 E+4 |  1.6 E+3 | SI 12 nT = 2035UT |
|18 March |   9 |  3-2-2-2-2-2-2-1  | 4.2 E+4 |  1.4 E+3 |                   |
|19 March |  14 |  1-2-2-3-4-3-3-3  | 2.3 E+4 |  1.6 E+3 |                   |
|20 March |  13 |  2-3-3-4-2-2-2-2  | 1.4 E+4 |  1.6 E+3 |                   |
|21 March |  18 |  1-1-2-3-5-3-3-2  | 9.6 E+3 |  1.5 E+3 | SI 25 nT = 0600UT |
|22 March |  19 |  2-3-4-4-3-3-3-4  | 1.1 E+4 |  1.6 E+3 |                   |
|23 March |  13 |  3-3-1-3-3-2-2-2  | 1.7 E+8 |  4.3 E+5 | Pro.Evnt.= 0820UT |
|24 March | 115 |  3-8-8-6-4-4-7-7  | 5.5 E+8 |  9.4 E+5 |SSC 184 nT= 0342UT |
|25 March |  92 |  6-8-5-6-6-5-5-6  | 2.4 E+7 |  8.2 E+3 |Severe Storm ; PCA |
|26 March |  83 |  6-6-7-6-6-5-5-4  | 1.2 E+7 |  1.4 E+4 |                   |
|27 March |  32 |  3-4-4-4-4-4-4-5  | 7.4 E+6 |  6.6 E+3 |                   |
|28 March |  20 |  3-4-4-3-4-3-3-2  | 3.8 E+6 |  3.3 E+3 |PCA Ended = 2300UT |
|29 March |   6 |  1-1-1-2-2-2-2-2  | 1.0 E+6 |  3.0 E+3 |Pro.Evnt. = 2120UT |
|30 March |  27 |  2-3-3-4-5-5-4-4  | 1.2 E+6 |  1.8 E+3 |Prot.Ended= 1215UT |
|31 March |  10 |  2-2-2-3-2-2-2-3  | 2.0 E+5 |  1.4 E+3 |                   |
 ----------------------------------------------------------------------------

NOTES:  Ap represents the planetary magnetic A-index for the day indicated.
  > 10 MeV represents the proton fluence for protons greater than 10 MeV.
 > 100 MeV represents the proton fluence for protons greater than 100 MeV.

**  End of Review **

------------------------------

End of SPACE Digest V13 #469
*******************