9 |
th Report: The CMO/OAA Observations made during a fortnight period from
An OAA Mars Section article to be published in
CMO #274 (
Masatsugu MINAMI, Director of the OAA Mars
Section
F |
rom this month we shall detail twice a month. From
D |
uring the period the observation time each night was about four
hrs possibly from 2 o’clock, the local time, to the time of Sunrise (at Okinawa
it was 5:45 JST at Naha on 28 June), and hence the Martian surface angle
observable from one fixed station was just about 190 degrees: From Asian and Oceanian regions the areas from M Cimmerium to Solis L were
observable, while in Europe they could catch the areas from Noachis to M
Sirenum, and in America from Solis L to Syrtis Mj. The tripod thus nearly
completes to cover globally the surfaces.
A |
lready the
AKUTSU, Tomio (Ak)
11 Sets of CCD Images (20, 21, 21,
f/32×32cm speculum with a
Bitran BJ-41L
ASADA, Tadashi (As) Munakata,
1 Set of CCD Images (
30cm SCT equipped with a
Panasonic NV-MX5000
BALDONI, Paolo (PBl)
Genova, Italia
1 Set of CCD images (
20cm SCT with a Philips ToUcam Pro
BATES, Donald R (DBt)
4 CCD Images (18, 19, 24,
f/21×25cm speculum with a Philips ToUcam Pro
BEISH, Jeffrey D (JBs)
12 Drawings (16,~20, 22, 23, 25,~27,
440, 570, 650, 870×41cm F/6.9
speculum
BUNGE, Robert (RBg) Bowie. MD,
4 Drawings (25,~27,
150, 250, 410×31, 43, 50cm specula
GRAFTON, Edward A (EGf)
6 Sets of CCD Images (17, 19, 20,
22, 23, 28 June)
f/27×35cm
Celestron with an ST5
HERNANDEZ, Carlos E (CHr)
1 Drawing (
ISHIBASHI, Tsutomu (Is)
3 B&W and Colour Photos (
31cm F/6.4
speculum; FCP400F, NP400P, HIE
&TP
KOWOLLIK, Silvia (SKw)
8 CCD Image
(16, 17, 21, 22, 25, 26,
18cm refractor with a Philips ToUcam Pro
KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan
4 CCD Images (20,
f/47×20cm
Dall-Kirkham with a Philips ToUcam Pro
LAZZAROTTI, Paolo R (PLz)
5 Sets of CCD Images (19, 22, 24, 25,
18cm Maksutov-Cassegrain with an Astromeccanica KC381
MELILLO, Frank J (FMl)
4 Red CCD Images (16, 24,
20cm SCT with a Starlight Xpress MX5
50 Drawings (20*, 21*, 23, 24, 26, ~30 June 2003)
*400×20cm refractor*/420, 530×25cm F/8.5 speculum
*
MOORE, David M (DMr)
5 Sets of CCD Images (17, 19, 21,
f/50×25cm speculum with an HX-5 or a Philips ToUcam Pro
MORITA, Yukio (Mo) Hatsuka-ichi,
7 Sets of CCD Images (10, 25, 26,
28,
f/50×25cm speculum equipped with an ST-5C
MURAKAMI, Masami (Mk)
3 Drawings (
NARITA, Hiroshi (Nr)
2 Drawings (
NG, Eric (ENg)
10 CCD Images (17, 18, 19, 22, 23,
24, 29,
f/35×25cm Royce
speculum with a Philips ToUcam
Pro
PACE, Ben (BPc)
2 CCD Images (19,
f/24×15cm Makstov with an HX516
PARKER, Donald C (DPk)
7 Sets of CCD Images (16, 19,
f/55×41cm F/6
Newtonian equipped with an ST-9XE
PELLIER, Christophe (CPl) Bruz,
9 Sets of CCD Images (16, 21, 24,
18cm Newtonian with a Philips ToUcam Pro
SEIP, Stefan (SSp)
2 CCD Images (22,
25cm Mak-Cass with a Philips ToUcam 740k
TAN, Wei-Leong (WTn)
2 Sets of CCD Images (18,
f/61,68×25cm Meulon with a Philips ToUcam Pro
TEICHERT, Gérard (GTc)
3 Drawings (19, 22,
Van Der VELDEN, Erwin (EVl)
1 CCD Image (
f/31×20cm SCT with a Vesta Pro modified
VALIMBERTI, Maurice P
(MVl)
3 CCD Images (22,
f/34×35cm
SCT with a Philips ToUcam Pro
WARELL, Johan (JWr)
7 Drawings (16, 17,
19, 22, 24, 26,
260, 400×25cm SCT (LX200)
3 Drawings (25, 26,
WILLIAMSON, Thomas E
(TWs)
2 Sets of CCD Images (27,
f/45×20cm
speculum with a Philips ToUcam
Pro
ZANOTTI, Ferruccio (FZt)
2 Sets of CCD Images (21,
40cm(à17cm) spec with a Philips ToUcam Pro
M |
orning and Evening Mists and Yellowish Haze: The phase angle ι was so large that it was hard to catch the evening whitish
mist, while it was rather thick near the evening terminator as observed by Mn on 27 June (λ=211°Ls) at
ω=095°W. The morning mist became quite evident from around 20 June
(λ=207°Ls): As Mn noticed on 20
June, the Martian surface appeared not reddish but rather yellowish. In fact,
the image made by VALIMBERTI (MVl) on
22 June (ω=208°Ls) at ω=140°W seems to
show an expansion of a yellowish haze over the morning brighter side. It is
thus quite possible for the white morning mist regarded as composing of water
vapour to be mixed now with the airborne dusts. On a different angle, PELLIER (CPl)’s image on 24 June (λ=209°Ls) at ω=241°W also
shows that a white –yellowish matter prevails over the morning
Evening
Mist at Æria: The evening mist sent to Aeria by an un-slope wind was reported in
a previous report, while this time the white cloud belt was also observed along
the northern coast of S Sabæus by PARKER (DPk) on 19 June (λ=206°Ls) ω=019°W, and
further westward by MOORE (DMr) on 25 June (λ=210°Ls) at ω=004°W.
Iapygia Viridis:
Dusts at Isidis Planitia: On 21June (λ=207°Ls) at ω=284°W, 290°W, CPl made images where a light dusty
matter is visible to the east side of Syrtis Mj. On the following 22 June (λ=208°Ls) at ω=259°W,
TEICHERT (GTc)
in
Later (on 7 July) they
published the image of the area of Isidis R to
http://www.msss.com/mars_images/moc/2003/07/07/
where the dust clouds at Isidis Planitia as well as at
Elysium. This also shows a spread of water vapour at Iapygia (at
Yaonis R
and M Serpentis: EGf’s image on 28 June above cited depict as well the bright aspect
of Yaonis R as well as the dark spots of M Serpentis. These aspects are also
comparable with the ones on the image made by MGS-MOC.
Details of M Cimmerium: It became now
rather apparent that M Cimmerium was of quite the same shape including several
spikes northward as observed in 1988: This period this fact is proven in the
images of ENg on 19 June (λ=206°Ls) at ω=195°W and of PLz on 30 June (λ=213°Ls) at ω=194°W, and so
on.
Eridania: Related with the report on Eridania in the preceding issue, a
thick morning mist patch near Eridania was caught by AKUTSU (Ak) on 21 June (λ=207°Ls) at ω=159°W.
According to Mn’s observations along
this angle on 20 June, the morning mist patch was considerably bright.
Region
around Solis L: DPk’s images on 16 June (λ=204°Ls) at ω=048°W~062°W
might be the first to scoop out newly the details of the dark markings around
Solis Lacus when δ=14.4". The eastern part of Solis L (including Helli Depressio?) is darker than
the other side, and the canal called Bathys is definite. Phasis is dark, broad,
rugged and curved, reminiscent of the aspects seen after the 2001 dust event.
Phoenicis L is definitely identified and Noctis L is
shown up as a dark spot. Notable is that Nectar is clearly curved down to Nia, and to its east, a light plateau, previously noted, is more evident. This particular rectangular light area may
correspond to Aurea Chersonesus
(or Aurea Cherso if we
employ the nomenclature of SCHIAPARELLI). It looks however slightly extended to
the south and Nia may be differently situated from
the one in the ANTONIADI-EBISAWA case [the present configuration is however not
so different from the one shown on the HST 1990 Red image filed as F673N which
was taken on
The area of Aurea Chersonesus came into sight
of our Oriental side observed around 26 June. The present writer (Mn) caught a detail of the area on 28
June (λ=212°Ls) at ω=057°W when δ=16.2", and on 29 June
(λ=212°Ls), he was blessed with a favourable seeing condition to observe
the area continually at ω=037°W, 047°W, 057°W, 067°W, 076°W, 086°W and
096°W. Otherwise Juventæ Fons
and a detail of Ophir were easily caught. Phasis was
dark and broad and curved to Solis L through Acampsis.
The ccd images were similarly produced by KUMAMORI (Km) and Mo on 26 June (λ=210°Ls) at ω=071°W, 081°W
(both by Km) and at ω=075°W (by Mo). On 28 June (λ=211°Ls), Mo took images at ω=057°W, and on 29 June (λ=212°Ls)
and 30 June (λ=213°Ls) ENg
produced excellent images at ω=094°W and ω=070°W respectively.
A detail of Auroræ Sinus, showing several canyons in a Lowellian way, is shown on the images by DPk on 16 June (λ=204°Ls) at ω=048°W and the
image of EGf
on 19 June (λ=206°Ls) at ω=038°W.
M Erythræum: As suggested in the preceding report, the dark
markings from Margaritifer S to its south-west look withered, and M Erythræum is narrower especially at the eastern part. This
is best shown this period on the image of EGf on 22 June (λ=208°Ls) ω=013°W.
Swelling of Orestes: There are visible
several spike-like projections along the northern coast of Margaritifer S to Auroræ S. Out of them, Orestes looks slightly expanded if we
scrutinise the area on EGf’s images
on 19 June (λ=206°Ls) ω=038°W and on 20 June (λ=206°Ls) ω=035°W as well as DPk’s images on 19 June (λ=206°Ls) ω=019°W (more
mildly processed).
Arsian White Cloud: The roll condensate cloud
associated with the evening Arsia Mons has been still active during this
period, and they were shown on the images made on 20
June (λ=207°Ls) by Mo at
ω=140°W as well as by Km at
ω=147°W and 151°W, and on 21 June (λ=207°Ls), Ak’s B showed it at ω=159°W. Similarly ENg at Hong Kong clearly showed it on 22 June (λ=208°Ls) at ω=143°W, and on 24 June (λ=209°Ls) at ω=149°W, and MVl at Melbourne caught it on 22 June (λ=208°Ls) at ω=119°W~140°W as
well as on 24 June (λ=209°Ls) at ω=127°W. The
latter image of MVl also shows Mons
Olympus clearly without any speck of cloud (might have been much better if R
and B were separately shot). On 28 June (λ=212°Ls) at ω=057°W the
present writer (Mn) saw a bright
stain near the morning limb which must have been Olympus Mons judging from the
apparent longitude & latitude angles.
The Arsia condensate
cloud appeared quite early in the afternoon: Mn saw it as a roundish white spot on 26 June
The SPC: a) Parva Depressio: As reported, the inside area of the south polar cap (spc) has
shown an interesting structural shadowy marking. To a naked eye, it is
sometimes caught not as just a shadowy dent but rather as a denser but narrower
rift segment which is confined quite inside. In the case of 1988 apparition, it
was on
If, as ANTONIADI
specified, Parva Depressio
is located at around Φ=75°S, it could be caught from the rear side since
φ=21°S. In this respect, DPk’s
images on 24 June (λ=209°Ls) at ω=328°W and 331°W
are very interesting and important. The spc on these images shows two groups of
dark areas: One is related with Rima Australis (to be
detailed below), but the other marking must be Parva
D. As a preceding case, also interesting is the configuration of the shadowy
details inside the spc on the image of EGf on 23 June (λ=208°Ls) at ω=010°W.
b) Thyles
Mons: On 24 June (λ=209°W) at ω=126°W, Mn
detected a bright protrusion from the perimeter of the spc near Parva D, and considered that this corresponded to a
rudiment of Thyles Mons. MVl’s
images on 24 June further show that the
“protrusion” is made of two bright lumps.
c)
Rima Australis: The rift next observed in 1988 was Rima Australis. In this apparition, this was already remarked by
DPk on a previous occasion. This time
the image by EGf
on 28 June (λ=211°Ls) at ω=302°W show
clearly Magna D and Rima Australis. These are also
apparent on BATES (DBt)’s image on
the same day at ω=314°W and otherwise HERNANDEZ (CHr), BEISH (JBs) and WHITBY (SWb)
observed visually on 26 June (λ=210°Ls) at ω=289°W, ω=314°W, and ω=323°W respectively. In
d)
Novus Mons: That Rima Australis
is present implies an appearance of Novus Mons. EGf’s image on 28 June (λ=211°Ls) at ω=302°W further
shows that there is a fragment attached to the outside of Novus Mons. The
fragment may be soon melted away, but interesting and it calls further
observations. DPk’s images on 24 June (λ=209°Ls) at ω=328°W and 331°W also
suggest the fragment.
e) Rudiments of
Argenteus Mons: According to ANTONIADI, Argenteus Mons
should be located around Ω=030°W and from Φ=62°S
to 78°S. The images of EGf on 18
June, 19 June, 20 June and 22 June show the rudiments of Argenteus Mons and
further his image on 23 June (λ=208°Ls) at ω=010°W more
clearly shows the germ of Argenteus Mons. From Japan, it came to sight around
from 27 June: The present writer (Mn)
caught visually on 28 June (λ=212°Ls) at ω=047°W, 057°W, 066°W on the
evening side, and also on 29 June (λ=212°Ls) at ω=028°W~057°W, and on
30 June (λ=213°Ls) at ω=018°W, 028°W: It was easy visually.
The NPH: DPk’s R image on 19 June (λ=206°Ls) at ω=019°W does not
show well the north polar hood (nph), but B image
shows the nph thickly (he uses the SBIG interference
B filter having the range 392 - 508nm). In general, however, the nph does not make a clear difference from the western limb
light since ι is large. An exception is the mildly processed MVl’s image on 22 June (λ=208°Ls) at ω=119°W ~140°W.
As described above, EGf
(ST-5C) showed the white nph as well as the yellowish
haze covering the morning limb side (partly the haze mixes with the white cloud
of the nph) on 23 June (λ=208°Ls) at ω=010°W.
PELLIER (CPl) has wisely begun from the beginning
of June in using the interference B filter of Type II (German made) to produce
fruitful results (CPl uses the ToUcam
in a B&W way, See LtE). On 24 June (λ=209°Ls) at ω=241°W, he thus
clearly separated the nph.
To shoot the nph, LRGB or RRGB is not appropriate. It is also not good
to skip the G ingredient. PEACH (DPc)
and others invented a good method to compensate by the use of a Magenta filter,
and ENg tried to employ the method on
17 June at ω=202°W, but we don’t hear
further news.
Images of this period: PARKER(DPk)’s set
of images made on 16 June (λ=204°Ls) at ω=048°W ~ 062°W is
impressive. Among many excellent images of GRAFTON (EGf), the image made on 22 June (λ=208°Ls) at ω=013°W should
be representative.
The
next issue
shall treat the period from 1 July
(λ=213°Ls) to
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