Mars Sketch (16)
from CMO #215 (10 April 1999)
As was stated several times, by the term Olympus Mons, we don't necessarily imply the crater itself of Olympus Mons. Often the mountain shows up itself when its summit or its frank is covered by a thick patch of white cloud, and then we sometimes just say Olympus Mons is visible. Classically this is quite identical with Nix Olympica, but unfortunately Olympus Mons and other Tharsis Montes are located differently from the areas in classical Martian Maps (see the Figure at p1386 in #144 for more details) and furthermore we don't have such a nomenclature as Nix something to Ascrĉus Mons and others. So we usually make use of the new terminology of Olympus Mons et al even if any is not exactly a summit or a crater of the mountains.
e have however encountered recently with a troublesome problem: As analysed in CMO #201 and #209, the very craters proved to be visible as densely reddish spots to us without presence of the orographic clouds in the early morning. We are therefore bound to discriminate between the clouded mountains and the summit without cloud.
By the same token, we should be
cautious when we use the terminology
The present writer observed on 31 Mar 1997 (098°Ls, δ=14.0", φ= 24°N, ι=11°) as follows:
Mn-464D ω=000°W v. poor->clouded
Mn-465D ω=019°W moderate
Mn-466D ω=029°W very poor
Mn-467D ω=048°W very poor
Mn-468D ω=058°W moderate
Mn-469D ω=068°W very poor
Mn-470D ω=078°W moderate->cloud coming
Mn-471D ω=092°W moderate
Mn-472D ω=102°W moderate
Mn-473D ω=112°W good
We here cite the drawings Mn-468D, Mn-470D, Mn-471D and Mn-473D which we believe show how the white patch developed when going into inside.
The Ascrĉus Cloud observed on 31 March 1997 by MINAMI by the use of a 20cm refractor
from left to right :
Mn468D(ω=058°W), Mn470D(ω=078°W), Mn471D(ω=092°W), Mn473D(ω=112°W)
The description in #188 implied the
coming white spot to be Ascrĉus Mons, but it should
be called the "Ascrĉus Cloud" or "Ascrĉus Mist" following Ascrĉus
Mons in the morning. From the view-point of ω, Mn-471D is comparable with
the HST image. We further note that the drawing Mn-441D cited in #201 was made
at ω=054°W (on
We did know in advance that the HST became in conjunction with us on the 30th day of March. We observed so the planet on the day also, but the seeing was poor though at ω=091°W we saw the white patch without much impression. (The patch was also seen at ω=064°W on 27 Mar also).
The local time of Ascrĉus Mons on the HST image on 30 Mar 1997 is about 10:30am as easily verified if we take into account ω=094°W, phase angle=11° (after opposition) and the Mons position ω=104°W (since (104-94+11)/15=1.4). Recent images of Don PARKER (on 30 Mar 1999), as shown in another column this issue, prove that Olympus Mons is already covered by the summit cloud at 10:40am, and so the time is possibly a very divide. The season is however different: it was 097°Ls on 30 Mar 1997 while 117°Ls on 30 Mar 1999. It is currently an interesting problem to know the time when each summit becomes orographically covered by cloud.
We furthermore have another problem of nomenclature: We thought the name Ascrĉus Lacus was renewed to Ascrĉus Mons. And so we often used instead the terminology Mareotis Lacus to denote the dark or densely reddish area preceding Olympus Mons. It was included in the schematic map in #188 p2050/51 where the "densely reddish" area was also defined. We therefore used Mareotis L for example in #190 at p2082. We are however now led to consider that the terminology Ascrĉus Lacus is still convenient and available to denote the densely reddish area around (110°W, 25°N).
(Mn : Masatsugu MINAMI)