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th Report:
The CMO/OAA Observations made during a fortnight period
from
1 October 2003 (271°Ls)
to
15 October 2003 (280°Ls)
An OAA Mars Section article to be published in
CMO #281 (25 October 2003 issue)
Masatsugu MINAMI, Director of the OAA Mars
Section
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ere
we review the Mars observations during the first half period of October 2003,
where the apparent diameter δ decreased from 20.7" to 17.9".
Since the maximal angular diameter in the 2001 apparition was 20.8", we
should say now the unprecedented opposition of Mars has ended. During the
present period, the Martian season proceeded from λ=271°Ls, just after the southern summer solstice, to
λ=280°Ls. The
previous great Mars in 1988 was closest to the Earth (on 22 September) when
λ=277°Ls, and hence
it is interesting to be aware that the present season corresponds to the season
of the 1988 Mars at opposition. At that time, the central latitude φ was
21°S, and this period φ was from 20°S to 22°S, and so nearly
identical. The phase angle ι increased from 26° to 33°.
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he observers and the
total observations were decreasing in number: ASADA (As) quitted shooting, and MORITA (Mo) was absent this period because his equator was out of order.
AKUTSU (Ak)’s
motor drive was also in trouble, and so his observations were vacant from 19
September to 5 October. The observers abroad became also inactive; Ch PELLIER (CPl) observed only two nights, while Don
PARKER (DPk) and Johan WARELL (JWr) were active
with productive results.
AKUTSU, Tomio (Ak)
7 Sets of CCD Images (6, 8, 9 October 2003)
f/33×32cm spec with a Bitran BJ-41L
BARNETT, John H (JBn)
2 Drawings (8, 13$ October 2003)
290,360×15cm Mak-Cass & 270,360×18cm refractor$,
$
BEISH, Jeffrey D (JBs)
1 Drawing (9 October 2003) 590×41cm F/6.9 speculum
BENAVIDES, Rafael (RBn) Córdova, España
6 CCD Images (5, 7, 9 October 2003) 24cm SCT with a ToUcam
3 CCD Images (6, 7, 9 October 2003)
f/25,30×23cm SCT with a TRV-900
BUDA, Stefan (SBd)
1 CCD Image (6 October 2003)
f/32×25cm Dall-Kirkhams with a ToUcam
BUNGE, Robert (RBg)
5 Drawings (2, 7, 8, 10, 14 October 2003)
249,480×43cm F/7.8 spec
CIDADÃO, António José (ACd) Œiras,
3 Sets of CCD Images (6, 10 October 2003)
25cm SCT with an FLI CM7-1E + AO2
COLVILLE, Brian (BCl)
1 Sets of CCD images (7 October 2003)
f/30×30cm SCTwith a ToUcam Pro
DOBBINS, Thomas A (TDb) OH,
4 CCD Images (3, 8, 13, 14 October 2003)
f/28×35cm SCT withToUcam & Wedge prism
FRASSATI, Mario (MFr) Crescentino (VC), Italia
1 Drawing (6 October 2003) 250×20cm SCT
FUMEGA UCHA, Camilo
(CFm) Ourense, España
1 CCD Image (8 October 2003)
f/25×31cm spec with a ToUcam
GRAFTON, Edward A (EGf)
3 Sets of CCD Images (11, 14, 15 October 2003)
f/39×35cm SCT with an ST-5C
IWASAKI, Tohru
(Iw)
10 Drawings (2, 4, 9 October 2003) 400×21cm speculum
KOWOLLIK, Silvia (SKw)
1 CCD Image (2 October 2003)
18cm
Starfire Refraktor with a ToUcam Pro
KUMAMORI, Teruaki
(Km)
11 CCD Images (1,
3#, 8#, 15 October 2003)
f/84×20cm Dall-Kirkham &
f/30×60cm Cass# with a ToUcam
#
MASSÓ MILLEIRO, Félix (FMr) La
4 CCD Images (4, 5, 10 October 2003)
15cm
F/8 Refr with a Quickcam
3000 Pro
MELILLO, Frank J (FMl)
5 Red CCD Images (4, 6, 10, 14 October 2003)
m SCT with a Starlight Xpress
MX5
MINAMI, Masatsugu (Mn) Fukui,
64 Drawings (2, 3, 4, 6, ~9, 12, 15 October 2003)
480, 400×20cm F/12 ED Goto
refractor*
*
MURAKAMI, Masami (Mk)
7 Drawings (9, 15
October 2003) 320, 400×20cm speculum
NAKAJIMA, Takashi (Nj) Fukui,
13 Drawings (2, 6, 9, 15 October 2003)
480, 400×20cm F/12 ED Goto refractor*
*
NARITA, Hiroshi (Nr)
11 Drawings (6, 9, 10, 15 October 2003) 400×20cm refractor
PARKER, Donald C (DPk)
24 Sets of CCD Images (4, 7, 9, 10, 13, 14 October 2003)
f/55, 59×41cm F/6 spec equipped with an ST-9XE or ToUcam
PEACH, Damian A (DPc)
Buckinghamshire,
5 Sets of CCD Images (10, 13, 14, 15 October 2003)
f/31×28cm
SCT with a ToUcam
PELLIER, Christophe
(CPl) Bruz,
4 Sets of CCD Images (7,
11 October 2003)
18cm spec with a modified B&W ToUcam Pro
SÁNCHEZ, Jesús
R (JSc) Córdova, España
3 Sets of CCD Images (8, 12, 14$ October 2003)
f/50×28cm SCT &
f/40×25cm spec$ with a ToUcam
SHERROD, P Clay (CSr) Aso Sky
2 CCD images (3, 15 October 2003)
f/35×41cm SCT with a ToUcam Pro
SIEGEL, Elisabeth (ESg) Malling, Danmark
5 Drawings (2, 4, 5, 11, 12 October 2003)
270×20cm F/10 SCT
TEICHERT, Gérard (GTc)
2 Drawings (13, 15 October 2003)
330×28cm SCT
VALIMBERTI, Maurice P (MVl)
6 CCD Images (3, 6, 10, 13, 14
October 2003)
f/34×35cm SCT with a ToUcam Pro
Van Der VELDEN, Erwin (EVl)
2 CCD Images (12, 15 October 2003)
f/31×20cm SCT with a Vesta
Pro modified
WASIUTA, Mylon
E (MWs)
1 CCD Image (8 October 2003)
f/30×15cm refr with a ToUcam
WARELL, Johan (JWr)
3 Drawings (2, 12,
14 October 2003)
260,
270×25cm SCT (LX200)
16 Sets of CCD Images (2, ~6, 9, 12, ~15 October 2003)
f/24×25cm SCT with a ToUcam
This Fortnight, the area from Solis L was well observed from
The Hole of the
Morning Condensate: In ##14 and 15, we took notice of a strange,
roundish de-concentration of the morning mist at Amazonis
which was first chased by Canon LAU (CLa) on 9 September 2003 (λ=257°Ls): This was still
preserved to this period, and checked by several ccd imagers. On 2 Oct (λ=272°Ls), WARELL (JWr) showed it at ω=120°W
(refer to the B image). This seemed a very nice moment to chase this
phenomenon, but unfortunately JWr’s preceding observation was made 20°W before, and no trace after the ω=120°W shot. The de-concentration was also checked on
6 Oct (λ=276°Ls) by
VALIMBERTI (MVl) at ω=123°W, and by AKUTSU (Ak) at ω=141°W: Ak’s case shows it when the Sun was
Wine-Coloured Ground. I: TDb’s image taken on 3 Oct (λ=272°Ls) at ω=041°W
shows generally an interesting reddish hue at the dark area preceding Thaumasia Fœlix down to S Meridiani and further eastward until Noachis.
It can be thus considered that the vast region is less covered by the airborne
dust and condensates now. DPk’s
images on 4 Oct (λ=273°Ls) at ω=017°W~077°W also show the wine colour distribution at the
dark area preceding Thaumasia though slightly
narrowly depicted than TDb’s.
They further show a wine coloured de-concentration of mist from Soils L toward
its north-west. These are also expected on the images by JWr on the day as noted above.
Visually the wine coloured area was watched generally
to the east of the Solis L region (eg by Mn on 9 Oct (λ=276°Ls) at ω=190°W etc). Moving to
Wine-Coloured Ground II:
Similarly, as noted in the previous issue, M Chronium
shows deeply a wine coloured hue. Km’s
images on 1 Oct (λ=271°Ls) at ω=200°W & 214°W prove it as well as MVl’s on 3 Oct (λ=272°Ls) at ω=163°W, on
6 Oct (λ=274°Ls) at ω=123°W, and
on 10 Oct (λ=277°Ls) at ω=132°W
etc: These show it runs quite eastwards. Ak’s image cited before made on 6 Oct also prove. The same region
shot on PEACH (DPc)’s
LRGB images taken later on 14 Oct (λ=279°Ls) at ω=195°W
also suggests the same colour. Visually the colour was evident to Mn as dark brown or brownish dark on 4
Oct (λ=273°Ls) at ω=166°W, 180°W, 195°W etc.
The Evening Limb: As the phase
angle ι has grown larger, the mist looked thicker and complex near the
evening limb under low sun illumination. At
Km
tried to enhance the whitish mist over the surface from around 8 Oct onwards. It was effective eg on the images taken on 15 Oct (λ=280°Ls) at ω=035°W~104°W. Visually the whitish mist became conspicuous around
from 12 Oct (λ=278°Ls), and on 15
Oct the present writer recorded that the white mist prevailed all over the
surface while the ground looked yellowish.
Morning
and Evening Condensates: In the preceding
issue, we pointed that the morning
(NB): Several LtEs in the preceding issue suggested that a dust
disturbance occurred at the area of
Mario FRASSATI’s Remark: MFr remarked on 6
Oct (λ=274°Ls) on his sketch at ω=249°W that there is a dust suspension
over the area near Ausonia. MASSO (FMr)’s ccd image on 5 Oct (λ=274°Ls)
at ω=267°W may also suggest similar
brightness. However we consider that this area just shows the ground lit in the
usual way. The present writer (Mn)
had occasions this time also to see the tetra-like area of Eridania and
southern Ausonia to be brilliant on 2 Oct (λ=272°Ls) at ω=203°W, 3 Oct
(λ=273°Ls) at ω=204°W and so on, but judged the area to be normal.
The TES result is also silent at this area.
Tom DOBBINS’ Remark: TDb sent us an email (13 October at 3:49 GMT) with his image
on 13 Oct (λ=279°Ls) at ω=295°W remarking "localized
brightening in
Surroundings of the SPC: Any description of the spc by ccd is uneventful
any more: No good images of Argenteus Mons and Rima Angusta are found: One of the best images are DPk’s R ingredients on 4 Oct (λ=273°Ls).
Its colour compositions destruct the perimeter, and even show a fringe of pure
red hue (being far from the wine colour). The contour of the spc should still
be paid attention, and sometimes a dark fringe was watched and still a cascade
seems to occur. For example, DPk’s
spc on 9 Oct (λ=276°Ls) at ω=319°W
shows partly a dark fringe, while the image on 10 Oct (λ=277°Ls) at ω=322°W does not. Both were
obtained by the same ToUcam. The spc on his true set of composite images by an ST-9XE on 9 Oct are not sharp because of B, but their R
components show well the interesting contour. The dark fringe of the IR image
of ACd’s
set on 6 Oct (λ=274°Ls) at ω=298°W looks similar to DPk’s on 9 Oct. EGf’s images on 11 Oct (λ=277°Ls) at ω=338°W
shows the dark fringe strongly. Beyond the fringe, any image proves that the
surroundings of the spc are faded in general, partly decoloured. TDb’s spc on 8
Oct (λ=276°Ls) at ω=347°W shows as if it
ejected a cascade.
From the side of
Note also that the southern high latitude area
near the terminator showed a white area misted or frosted: Mn’s records are as follows: on 2 Oct (λ=272°Ls) at ω=174°W(Thyle II light?), on 3 Oct (λ=273°Ls) at ω=175°W, on 4 Oct (λ=273°Ls) at ω=166°W, 180°W, on 6 Oct
(λ=274°Ls) at ω=137°W, 147°W, on 7 Oct
(λ=275°Ls) at ω=138°W, 157°W, on 8 Oct
(λ=276°Ls) at ω=099°W, 109°W, 119°W (light in O56, but dull in G), on 9 Oct (λ=276°Ls) at ω=159°W, on 12 Oct (λ=278°Ls) at ω=104°W, and on 15 Oct (λ=280°Ls) at ω=025°W, 034°W, 044°W, 054°W, 073°W, 083°W, 098°W.
Relic of Novus Mons: Novus Mons already vanished as noted in a previous report but still the
place where its ice presented or the trench is still identified. For example, DPk’s R images on 9 Oct (λ=276°Ls) at ω=333°W hint the place as decoloured. EGf’s image on 14
Oct (λ=279°Ls) at ω=314°W also suggests the segment.
Maurice VALIMBERTI’s Remark: MVl sent us an email on 15 Oct at
15:30GMT suggesting that there is "a brightening at Southern latitudes from
around Argyre to southern Dia & across to Noachis." The brightening is not so explicit or
evident to us as far as we see his images on 14 Oct (λ=279°Ls) at ω=050°W et
al, while it is certain that the area around Dia down
toward the EN shows a sandy colour. This kind of surface nature might be the
same as that seen outside the area where the decay of Thyles Mons took place.
The present writer similarly recorded on 15 Oct (λ=280°Ls) at ω=054°W, 073°W, 083°W that there was seen a broad sandy band from the
southern high latitude terminator to the EN direction; regarding this as a kind
of fallout.
Olympus
On the other hand, it is known that Arsia Mons continues
to suffer from the condensate activity in the evening for a long time and should
be supposed to be clouded up to this season. The Arsia cloud really once
decreases at around λ=230°Ls, but soon
becomes reactive from before the southern summer solstice. In 1988, at this
period Arsia Mons was vivid in B while Olympus
However, this time the sunset line is already away
to the rear side, and even if we pick out the Arsia Mons on MVl’s afore-cited image taken on 3 Oct
(λ=273°Ls) at ω=163°W, it is still near
at 1 o’clock PM (taking account ι=27°, and Arsia Mons’s longitude at Ω=120°W), and we can never say it’s in the evening. Even
if Arsia Mons be on the limb, it must be just two hrs before the sunset, and
hence we have to be much careful to the limb side. That is, we need good B
images of ω=180~200°W.
Unfortunately we have not had pertinent images.
Furthermore, as a general tendency, the more the phase angle increases, the more
uncleared becomes the limb side of the ccd images. The present writer (Mn) visually observed on 4 Oct (λ=273°Ls) at ω=195°W (ι=28°) the limb side by the use of G filter: The limb
was misty bright, but he could not identify the distinguished spot. The
detection of the Arsia cloud at this season may be thus a theme handed over to
2005. In 2005, the southern summer solstice comes before opposition, and so
observable though the angular diameter is not enough (around 14”).
NPH: Since the
winter solstice came in the northern hemisphere, the behaviour of the north
polar hood might be interesting (according to W H PICKERING, the nph is thick
but the npc is not completed). However
this period few special activities were observed. DPk’s images on 4 Oct (λ=273°Ls) at ω=017°W~077°W show well the nph covering M Acidalium. Note
however the northern part of M Acidalium is seen through: On his R image, the
district around 55°S is quite
dark, not snowed. JWr’s
images on 9 Oct (λ=276°Ls) at ω=039°W also depict well
the nph, and on R, the northern end is dark. MVl’s description of the nph on 14 Oct (λ=279°Ls) at ω=050°W looks very real in
density of the nph. Nothing in particular however in other
longitudes.
Occultation of Mars on 6 October 2003: On 6 Oct,
Mars was seen to be occulted by the Moon at Oceania including
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he next
issue shall treat the observations made in the Second half of October 2003 from
16 October (λ=280°Ls, δ=17.8") to 31 October 2003 (λ=290°Ls, δ=15.1").
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