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
rom this month we shall detail twice a month. From
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.
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,
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,
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
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
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
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.
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,
Later (on 7 July) they
published the image of the area of Isidis R to
where the dust clouds at Isidis Planitia as well as at Elysium. This also shows a spread of water vapour at Iapygia (at ); this corresponding to the observation by SWb on 30 June (see above).
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.
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.
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
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.
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.
shall treat the period from 1 July