20 |
th Report:
The CMO/OAA Observations made
during a fortnight period
from
1 December
2003 (308°Ls)
to
15 December 2003 (317°Ls)
An OAA Mars Section article to be published in CMO #285 (25
December 2003 issue)
Masatsugu MINAMI, Director of the OAA Mars Section
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his time we review
the CMO Mars observations made during the period from 1 December (λ=308°Ls) to 15 December
(λ=317°Ls): This period was important because it meant still the Martian
season for dust storms as stressed by R McKim (RMk) on 18 November (#283 LtE).
However since the apparent diameter δ decreased from 11.1" to
9.7", routine observers much decreased. In Japan the typical winter
climate prevailed: but fortunately those who faced to the Pacific Ocean like
Tomio AKUTSU (Ak) and Teruaki KUMAMORI (Km)
were quite active, while those living at the rear side (eg
at Fukui) had less opportunity to watch. During the period, the central
latitude φ was 26°S, and the phase angle ι =42°. The expected dust
storm was clearly detected by Don PARKER (DPk) on 13 December (λ=315°Ls)
when δ=9.9".
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he observers who
contributed this time are as follows: Elisabeth SIEGEL (ESg) in
AKUTSU, Tomio (Ak) Karasuyama,
7 Sets of CCD Images (+19 IR image)
(3, 8, 10, 13, ~15 December 2003)
f/33×32cm spec with a Bitran BJ-41L
BENAVIDES, Rafael (RBn) Córdova, España
2 CCD Images (
BIVER, Nicolas (NBv)
2 Colour Drawings (9, 15 December
2003) 510×26cm spec
CAPARRÓS, Angel (ACp)
Málaga, España
1 CCD Image (12 December 2003)
F/4.8 25cm spec with a ToUcam
COLVILLE, Brian (BCl) Ontario, Canada
1 Set of CCD images (14 December
2003)
f/44×25cm SCT with a
ToUcam Pro
COOPER, Jamie (JCp)
1 CCD Image (15 December 2003)
f/30×18cm Intes-Micro Mak-N with
ToUcam
GRAFTON, Edward A (EGf)
1 Set of CCD Images (15 December
2003)
f/39×35cm SCT with an
ST-
IWASAKI, Tohru
(Iw)
5 Drawings (2, 4 December
2003) 400×21cm speculum
KARRER, Michael (MKr) St Radegund, Österreich
1 CCD Image (9 December 2003)
f/35×18cm Meade Refraktor with a ToUcam
KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan
13 CCD Images (2, 3#, 4#,
9#, 10#, 14#
December 2003)
f/84×20cm
Dall-Kirkham & f/40×60cm Cass#
with a ToUcam
#
MELILLO, Frank J (FMl)
1 Red CCD Image (5 December 2003)
20cm SCT with a
Starlight Xpress MX5
MINAMI, Masatsugu (Mn)
Fukui,
14 Drawings (5, 10 December 2003)
600, 480, 400×20cm F/12
ED Goto refractor*
*
MURAKAMI, Masami (Mk)
11
Drawings (2, 10, 14, 15 December 2003) 320, 400×20cm spec
NAKAJIMA, Takashi (Nj)
Fukui,
2 Drawings (
*
PARKER, Donald C (DPk)
7 Sets of CCD Images (5, 9, 13, 14*
December 2003)
f/55, 59×41cm F/6 spec equipped with an ST-9XE/
*f/19×32cm SCT with
a ToUcam
(with
T D'AURIA and
PEACH, Damian A (DPc) Loudwater,
1 Set of CCD Images (+ 5 Set
Images) (9, 15 December 2003)
f/31×28cm SCT with
an ATK-1HS
PELLIER, Christophe (CPl) Bruz,
1 Set of CCD Images (+3 IR+B Images)(7, 14+,
18cm spec/35 cm SCT+ with a modified B&W ToUcam Pro
SIEGEL, Elisabeth (ESg) Malling, Danmark
4 Drawings (6, 9, 10,
TEICHERT, Gérard (GTc)
3 Drawings (7, 8,
Van Der VELDEN, Erwin (EVl)
3 CCD Images (1, 10, 12 December
2003)
f/31×20cm SCT with a Vesta Pro modified
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he
Minimal South Polar Cap: On 5 Dec
(λ=311°Ls), DPk gave nice R images at ω=111°W, 117°W where the spc is
shot small but clearly: As suggested by T SAHEKI long time ago the season at
λ=310°Ls is critical, and so we can regard the R image of the spc on DPk’s
as a final residual one. ESg also felt the
spc was as if suddenly small on 6 Dec after the preceding observation on 28
November: On 9 Dec (λ=313°Ls) at ω=324°W she observed a circumpolar
polar haze from 30°S southward by Int.
IR Images before Sunset: Ak obtained on 8 Dec (λ=312°Ls) an IR image at before
DPk’s Detection of a
Significant Dust Storm on 13 Dec (λ=315°Ls): A clear large dust
storm was found by DPk on 13 Dec at ω=072°W (01:35GMT) which expanded
from Chryse to the wider area around Eos, covering
half of Aurora S, further detouring to Candor, and
southwardly reached the northern part of Argyre,. DPk also suggested
another core at
On the following 14 Dec (λ=316°Ls), DPk
produced an image with D'AURIA and FAWORSKI at ω=044°W (00:19GMT), and
COLLVILLE (BCl) in Canada at ω=047°W (00:30GMT): The dust looked largely
expanded or stayed at higher altitude, and showed several new dust cores at
Eos, Capri Cornu, and also at the west of Argyre. On the day Ak
succeeded in catching the west end of the dust at ω=111°W (4:56GMT=13:56JST) in IR, and
KUMAMORI (Km) also caught it at ω=118°W(5:23GMT=14:23JST)
by the use of R-640. The western end of the dust was near the centre of Solis
L, and the southward end reached to the west of Aonius
S making a bright core. Ak was eventually able to
compose an RGB image at ω=145°W (7:15GMT=16:15JST), where the core
was light also in B. Ak also visually checked it at
around
On the evening, Ak readily processed, and
sent the images to us at
On 15
Dec (λ=316°Ls), GRAFTON (EGf) made a set of clear images at ω=038°W (00:36GMT): The dust at high
altitude seemed to be remnant to the extent that the western half of S Sabaeus
as well as Meridiani S were faded, and a bright new core was seen to the south
of Aram, and bright belt to the east of Argyre, and
also several small cores at Eos and Capri Cornu. It was notable however that
the lowlands of Niliacus L and M Acidalium were not
deformed and looked as usual, and just haunted by a white haze independent of
the dust cloud. Further notable was that the B image showed a bright core at
the morning Argyre and its west implying a condensate patch associated with the
dust.
In
MGS-MOC
Observations: Apparently the images of DPk
on 13 Dec shows that the dust storm is slightly not fresh considering the
expansion: Really the dust chart on the preceding 12 Dec (λ=314°Ls) made
by TES (http://tes.asu.edu/dust/dust.mov) shows already a rise of dust cores near Chryse and Eos. The MGS-MOC wide angle images, shown here,
prove certainly a full of dust at the southern Chryse
and Eos to Valles Marineris.
The MOC images also show several dust distributions on the preceding days, but
as far as we depend on the TES images we may be suggested to regard that the
essential dust having a potential remnant dust was onset on 12 December. As
repeatedly we stress, the Martian dust disturbance does never propagate like
the Hurricanes or Typhoons, and the initial latent one rather
subsides at the night side, and makes a new one rise in the next morning
discontinuously (maybe at a different place), and so we cannot easily trace the
relationship among several dust disturbances before 12 Dec. TES suggests a dust
disturbance near at Tempe on 4 Dec (λ=310°Ls), and it became again latent
next day, but this may be regarded as a precursor, and may be said to have
developed to the cross-equatorial dust storm in a week.
The TES image on 15 Dec proves the position of the south-western end of
the dust as well as an existence of a bright core near Dia
which matches the observations by Mk and Ak
on 15 Dec. The MGS observations are made at 2 o’clock PM, while terrestrial
observations show well the morning side: It is interesting and may be important
to see that the morning condensates are conspicuous at the latitude around 60°S
while the afternoon TES shows a new steady core at around the area of Dia.
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he next
issue shall treat the observations made in the Second half of December 2003
from 16 December (λ=317°Ls)
to 31 December 2003 (λ=326°Ls, δ=8.5").
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