10th Report: The CMO/OAA Observations made during a fortnight period from

1 July 2003 (213Ls) to 15 July 2003 (222Ls)


An OAA Mars Section article to be published in CMO #275 (25 July 2003 issue)


Masatsugu MINAMI, Director of the OAA Mars Section


Japanese version here


W

e here review the Mars observations made during the fortnight period from 1 July 2003 to 15 July 2003, when the Martian season proceeded from λ=213Ls to 222Ls. The data were well comparable with those obtained by Viking Orbiter 2 in 1977. The south polar cap (spc) well thawed in such a way that its perimeter lay between 60S and 70S.

The central latitude φ kept 21S, and the phase angle ι went down from 37 to 32. The apparent diameter δ grew from 16.7" up to 19.2". The diameter of 19 arcsecs was not experienced from 1990 to 1999, and we shall also not be able to experience at the oppositions from 2007 to 2016. So we were already quite in season of the red planet, while unfortunately the rainy season did not leave from the Japan islands yet.

 

T

he Japanese main island was suffering from the rainy season, while MORITA (Mo) and KUMAMORI (Km) tried to be active. VALIMBERTI (MVl) was on standby but the winter sky prevailed at Melbourne. The weather at Florida, Hong Kong and Okinawa was favourable. PELLIER (CPl) and LAZZAROTTI (PLz) were also productive, and KOWOLLIK (SKw) became well in tune. HEATH (AHt) started from 10 July, SIEGEL (ESg) from 11 July and GRAHAM (DGh) from 15 July. Forty-four observers contributed including ten Japanese observers.

Incidentally, the apparent declination of the planet was about -13.5 to -13, and so at this period the planet Mars at meridian shined seen from Denmark at the altitude of 21 while from Singapore at about 75. Other examples: CPl was able to catch Mars at meridian at the altitude of 29, PLz of 34, Mo and Km of 43, Mn (Okinawa) of 51, DPk (Florida)of 52, ENg (Hong Kong) of 55, MVl (Melbourne) of 65.

AKUTSU, Tomio (Ak)  Tochigi, Japan

5 Sets of CCD Images (4, 15 July 2003)

f/3232cm speculum with a Bitran BJ-41L

 

ASADA, Tadashi (As) Munakata, Fukuoka, Japan

5 CCD Images (9, 15 July 2003)

30cm SCT equipped with a Panasonic NV-MX5000

 

BALDONI, Paolo (PBl)  Genova, Italia

3 CCD images (6, 12, 13 July 2003)

18cm Intes-Micro Gold F6 with a ToUcam Pro

 

BATES, Donald R (DBt) Houston, TX, USA

6 CCD Images (2, 6, 11, ~14 July 2003)

f/2125cm speculum with a ToUcam Pro

 

BEISH, Jeffrey D (JBs) Lake Placid, FL, USA

16 Drawings (1,~11, 13, 15 July 2003)

440, 570, 650, 87041cm F/6.9 speculum

 

BIVER, Nicolas (NBv) Versailles, France

2 Colour Drawings (10 July 2003) 41026cm speculum

 

BUNGE, Robert (RBg) Bowie. MD, USA

6 Drawings (2, 4, 5, 6, 12, 15 July 2003) 150, 250, 41031, 43cm specula

 

COLVILLE, Brian (BCl)  Ontario, Canada

1 CCD image (2 July 2003) 30 cm SCT with a ToUcam Pro

 

CORDIALE, John E (JCd) Hudson Falls, NY, USA

1 Set of CCD Images (1 July 2003) 25 cm Meulon with a ToUcam Pro

 

FRASSATI, Mario (MFr) Crescentino, Italia

1 Set of Drawings (13 July 2003) 250, 40020cm SCT

 

GRAFTON, Edward A (EGf) Houston, TX, USA

9 Sets of CCD Images (2, 3, 6, 8, ~13 July 2003)

f/2735cm SCT with an ST-5C

 

GRAHAM, David (DGh) North Yorkshire, UK

1 Colur Drawing (15 July 2003) 17010cm refractor

 

HEATH, Alan W (AHt) Nottingham, UK

2 Drawings and 1 Note+ (10, 13+, 14 July 2003)

20020cm SCT/+17525cm spec

 

HERNANDEZ, Carlos E (CHr) Miami, FL, USA

       2 Drawings (7, 11 July 2003) 250, 37023cm Maksutov-Cassegrain

 

ISHADOH, Hiroshi (Id) Naha, Okinawa, Japan

       1 CCD Image (4 July 2003) 31cm speculum attached with a Canon G2

 

ISHIBASHI, Tsutomu (Is) Sagamihara, Kanagawa, Japan

1 Set of B&W and Colour Photos (15 July 2003)

31cm F/6.4 speculum; FCP400F, HIE

 

KOWOLLIK, Silvia (SKw) Stuttgart, Deutchland

30 CCD Images (4, 7, 10, 11 15 July 2003)

18cm refractor with a Philips ToUcam Pro

 

KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan 

11 CCD Images (2, 7, 10, 11, 15 July 2003)

f/4720cm Dall-Kirkham with a ToUcam

 

LAZZAROTTI, Paolo R (PLz) Massa, Toscana, Italia

6 Sets of CCD Images (7, 8, 11, 12, 13, 15 July 2003)

          18cm Maksutov-Cassegrain with an Astromeccanica KC381

 

MELILLO, Frank J (FMl) Holtsville, NY, USA

      7 Red CCD Images (2, 5, 8, 9, 13, 15 July 2003)

20cm SCT with a Starlight Xpress MX5

 

MINAMI, Masatsugu (Mn) Naha, Okinawa, Japan

105 Drawings (1, ~15 July 2003) 420, 530, 55025cm F/8.5 speculum

 

MOORE, David M (DMr) Phnix, AZ, USA

3 Sets of CCD Images (8, 11 July 2003)

f/5025cm speculum with an HX-5 or a Philips ToUcam Pro

 

MORITA, Yukio (Mo) Hatsuka-ichi, Hiroshima, Japan

8 Sets of CCD Images (1, 3, 6, 10 July 2003)

f/5025cm speculum equipped with an ST-5C

 

MURAKAMI, Masami (Mk) Yokohama, Kanagawa, Japan

      51 Drawing(s) ((10), 15 July 2003) (320), 40020cm speculum

 

 

NARITA, Hiroshi (Nr) Kawasaki, Kanagawa, Japan

1 Drawing (4 July 2003) 40020cm refractor

 

NG, Eric (ENg) Hong Kong

17 CCD Images (1, ~9, 12, ~15 July 2003)

f/3525cm Royce spec with a Philips ToUcam

 

PARKER, Donald C (DPk) Miami, FL, USA

15 Sets of CCD Images (1, ~4, 6, 8, 13 July 2003)

f/5541cm F/6 spec equipped with an ST-9XE

 

PAU, K C (KPa) Hong Kong

3 CCD Images (1, 2, 5 July 2003)

21cm spec (CN212) with a ToUcam Pro

 

PELLIER, Christophe (CPl) Bruz, Ille-et-Vilaine, France

21 Sets of CCD Images (3, 5, 6, 8, 10, ~14 July 2003)

18cm Newtonian with a modified B&W ToUcam Pro

 

ROEL SCHREURS, Eric (ERl) Mexico

1 CCD Image (13 July 2003) 25cm TEC Maksutov with a ToUcam

 

SNCHEZ, Jess R (JSc) Crdova, Espaa

1 CCD Image (15 July 2003) 28cm SCT with a ToUcam

 

SCHMUDE, Richard W, Jr (RSc)   GA, USA

2 Drawings (3, 10 July 2003) 153, 23010cm refractor

 

SEIP, Stefan (SSp) Stuttgart, Deutchland

1 CCD Images (10 July 2003)

25cm Mak-Cass with a Philips ToUcam 740k

 

SHERROD, P Clay (CSr) Aso Sky Observatory, AR, USA

16 CCD images (3, ~10, 13, 14, 15 July 2003)

41 cm SCT with a ToUcam Pro

 

SIEGEL, Elisabeth (ESg) Malling, Danmark

4 Drawings (11, 12, 13, 15 July 2003) 27020cm F/10 SCT

 

TAN, Wei-Leong (WTn) Singapore

5 Sets of CCD Images (5, 8, 15 July 2003)

f/61,6825cm Meulon with a ToUcam Pro

 

TEICHERT, Grard (GTc) Hattstatt, France

3 Drawings (10, 11, 15 July 2003) 33028cm SCT

 

Van Der VELDEN, Erwin R (EVl) Brisbane, Australia

7 CCD Images (3, 14 July 2003)

f/3120cm SCT with a Vesta Pro modified

 

VALIMBERTI, Maurice P (MVl) Melbourne, Australia

3 CCD Image (2, 8 July 2003)

f/3435cm SCT with a Philips ToUcam Pro

 

WAKUGAWA, Tetsuo (Wk) Kochinda, Okinawa, Japan

      15 CCD Images (6, 9, 10, 12, 14 July 2003)

40cm speculum equipped with a Sony VX-1000

 

WARELL, Johan (JWr) Tcuson, AZ, USA

       3 Drawings (3, 7, 9 July 2003) 260, 40025cm SCT (LX200)

 

WHITBY, Samuel R (SWb) Hopewell, VA, USA

3 Drawings (7, 9, 19 July 2003) 31015cm speculum

 

WILLIAMSON, Thomas E (TWs) Alburquerque, NM, USA

4 Sets of CCD Images (4, 12 July 2003)

f/4520cm spec with a Philips ToUcam

 

ZANOTTI, Ferruccio (FZt) Ferrara, Italia

3 CCD Images (1, 6, 8 July 2003)

40cm(17cm) spec, 18 cm MC with a ToUcam Pro

 

D

ust Clouds: A review from 21 June (λ=207Ls) to 30 June and 1 July (λ=213Ls): As reviewed in the preceding report, a sign of dust plume germ checked by PELLIER (CPl) on 21 June (λ=207Ls) at ω=284W, 290W at the eastern coast of Syrtis Mj finally triggered a mixed atmosphere up to the area of Iapygia Viridis observed by WHITBY (SWb) on 30 June (λ=213Ls) at ω=286W. The area of M Tyrrhenum looked also faded. On 1 July (λ=213Ls), a further condensation of mixed dust was seen at Iapygia Viridis: The mildly processed image by CORDIALE (JCd) (processed by David MOORE (DMr)) on 1 July (λ=213Ls) at ω=273W shows it and also does that the higher atmosphere was quite dirty. PARKER (DPk)s images on the day at ω=273W was made to figure the condensed part. A branch of dust near the Huygens crater is more evident on DPks images. The general configuration of the dust covering over the area around M Tyrrhenum may well be checked by a comparison of JCds image with CPls previous image taken on 24 June at ω=263W. BEISH (JBs) observed the condensed part on 1 July (λ=213Ls) at ω=267W (9:00GMT) and suggested that S Sabus had already been washed out. This observation was communicated from MURAKAMI (Mk) to Okinawa at 11:13 GMT, and so ISHADOH (Id) and the present writer (Mn) were on alert at Ameku, Naha, Okinawa. The planet came out to be observed just before the midnight (15hrs GMT), while S Sabus was normally dark and no sign of dust disturbance over there. So at mid-night, Mk uploaded the following message on the Faade of the CMO-Web: 01 July at 15 hrs GMT: (1st Temporary Report concerning BEISH's observation at 9 hrs GMT) Mars has just come above the eastern horizon from Japan, and ISHADOH (Id) and MINAMI (Mn) at Naha have just checked the area of S Sabus. The planet is still quite low but both can detect the usual presence of the evening S Sabus by the use of a 25 cm spec at 230x as well as a 25cm Meade at 280x. They will soon begin routine observations. Mns routine observation started from 15:50 GMT the night, and Id stayed with Mn and drew two sketched at 16:10 and 16:50GMT by the use of the WAKUGAWA(Wk)s 25 cm Newtonian. There was no abnormality seen from our side.

 

 2 July (λ=214Ls): The Martian season came up to the particular dusty season when S EBISAWA and A DOLLFUS discovered a clear dust condensation in 1971 on 11 July at Meudon. The dust at that time was seen at Noachis in bar-like form Yaonis R down to S Sabus. This dense 1971a however lost its power to reproduce soon at λ=215Ls. On 2 July 2003, there were made many observations in the US, and they proved that the Iapygia condensation appeared to have been reproduced brighter. JBs observed at ω=249W~272W, DPk at ω=262W, 266W, MELILLO (FMl) at ω=266W, GRAFTON (EGf) at ω=268W, BATES (DBt) at ω=275W et al. The processing varies since the yellow overall dust prevails, but we here show a comparison of the image by DBt on 2 July with JCd on the preceding day.

JBs sent out an alert on 2 July 19:16 GMT. However the observations on 2 July at Naha showed still no happenings at the Noachis site. On the other hand, Achillis Pons was clearly seen because of a present of a dust streak, and its west end was quite dusty and showed a heart shaped dusty patch. This was clearly shown on KUMAMORI (Km)s images at ω=009W, 028W, VALIMBERTI (MVl)s at ω=016W, KC PAU (KPa)s at ω=025W, and Eric NG (ENg)s at ω=050W, 059W. This was also checked by Id and Mn at Naha (as noted on the Faade as Directors Note on 2 July): The sky at Ameku was fine up to ω=038W (at 18:30 GMT) but then Mn was annoyed by cloudy conditions, while the sky was good at Shuri, and Id continued to check it until 19:50 and 20:30 GMT. The observation by MVl was sent at 19:44 GMT, and Mn wrote a reply at 22:53 GMT (about the similar phenomenon observed in 1986 at λ=225Ls when a dusty matter went up from the north polar region to Chryse), and at the same time asked Mk to upload MVls image on the Faade of the CMO-Web.

 

3 July (λ=215Ls): The Chryse cloud however did not repeat on 3 July so much: Just Achillis Pons was evident because of a yellow streak and the area looked dirty (see Van der VELDEN(EVl)s images at ω=002W, 020W and 039W). The area of Noachis proved also unchanged. The comparison of DPks image on 3 July with the one on 2 July at ω=262W shows that the Iapygia cloud was slightly spread, but the 3 July image newly shows a dust plume at the northern Yaonis R. EGfs R image (milder than the L) at ω=261W further shows also a lower streak from Iapygia to the direction of M Serpentis, while S Sabus is well seen as on 2 July. Ausonia Borealis looks rather normal though slightly obscure; and the dusty cloud without cores looks to have spread to the east. Visually WARELL (JWr) caught the Iapygia core at ω=280W.

 

4 July (λ=215Ls): Referring to the images by SHERROD (CSr) at ω=245W, 253W, by DPk at ω=244W, 254W, and by WILLIAMSON (TWs) at ω=250W, 266W, the Iapygia core moved to Hellas and also developed to the west. This arm is more evident in DPks B and so must be a condensate. Otherwise, another weaker arm goes down on B and G from the eastern end of Iapygia Viridis to the direction of the east-southern part of Syrtis Mj. This was not seen on 3 July nor also later on 6 July. The condensate streak which lies from M Tyrrhenum to M Cimmerium is still seen but weaker than on 3 July.

On 4 July the last image produced in the US was the one made by TWs at ω=266W (at 10:43 GMT) where it is shown a dusty matter at M Serpentis which also crosses the eastern S Sabus. The phase angle was ι36 on the day, and so the early morning side is at the rear side by more than two hrs.

The dust germ was observed 4 hrs later at Okinawa after the wall of the Pacific Ocean. The planet was still low but by 15h GMT (midnight JST), ISHADOH (Id) and Mn confirmed independently the new occurrence of the conspicuous dust disturbance over the eastern part of Deucalionis R which was curved down to smear out the eastern part of S Sabus. It readily reminded us of the 1971a. [Next morning, we heard MIYAZAKI (My) at Gushikawa, Okinawa also observed the clear dust cloud just after 14h GMT by the use of the famous 40 cm reflector. Since from his observatory, there is no obstacle to conceal the eastern horizon, he must be the first to notice the disturbance, while the rooftop at Ameku where Wks 25 cm spec was set was surrounded by a balustrade which was too annoying to look the horizon.] The seeing condition became stable after 15h GMT enough to begin to make a sketch, and Mn produced the first drawing at 15:30 GMT (from 15:20 to 15:40 GMT). Before that, Mn real-timely emailed to Mk at 15:10 GMT about the dust occurrence and Mk uploaded the news readily on the Faade of the CMO-Web. The present writer (Mn) chased the dust cloud succeedingly at 16:10, 16:50, 17:30, 17:50, 18:30 GMT (still ω=019W). It should be remarked that while the new dust cloud was bright and clear, the evening side was largely obscured by the yellow haze, and the morning side was also misted deep to the area of S Meridiani. The shape and brightness of the clear curved dust did not change until it went away to the rear side. By 20:10 GMT (at ω=044W), the dust had been completely concealed. Id at Naha took a picture of the cloud at 16:28 GMT (ω=350W) by the use of a Canon digital camera. AKUTSU (Ak) at Nasu near Tokyo took a set of images in a lull of the cloudy weather at 17:04 GMT (at ω=358W), but the seeing was too poor to shoot the dust cloud. At Melbourne, MVl was also on alert from the lower planet at the altitude of 1020, and took a glimpse of the timing surface at 13:02 GMT, but as he emailed to us at 18:00 GMT (4 oclock Australian Time), the winter sky prevailed throughout the night (MVl wrote I have stayed up most of the night in the hope of the sky clearing, but it looks as if this will not happen). The present writer (Mn) wrote a report before the last observation at 20:20 GMT, and sent it to Mk: Mk at cmo@ then forwarded it to the CMO members at 19:59 GMT (4:59 JST) as CMO 2003 News #1. It partly informed "Tonight, at 15 hrs on 4 July 2003 GMT,.. both (Id and Mn) readily noticed a new emergence of a bright arched belt of dust having a sharp boundary at the eastern part of Deucalionis Regio, and its branch erased clearly the eastern part of S Sabus. The rest of S Sabus and S Meridiani remained dark. The area just went away into the evening thick mist at around 18:30 GMT, without changing its shape and brightness. Compared with our observations yesterday, this was a new aspect. " At 21:47 GMT, ENg at Hong Kong sent images at 20:56 GMT (at ω=055W), while he had missed the midnight dust disturbance. In the evening Mn met with HIGA (Hg) at Naha, but Hg also said he had just observed no more than the morning planet.

 We shall make a detailed report of the new dust occurrence and the subsequent development much later after the season ends, but close for now just by mentioning the following characteristic of the 4 July phenomenon: The uncovered part of S Sabus, namely the western area of S Sabus looked outstanding in density and colour as well as S Meridiani. The remaining part was particularly dark in a deep chocolate colour. This was considered because the preceding dusty area was disturbed by the ascending air current while the atmospheric pressure of the following part was so high to supply the lower air to the dusty area. The area lying under the high pressure atmosphere must look more transparent. From the following day, there occurred an intermixture and S Sabus recovered totally but the colour and density appeared different and weaker. The transparency turned to be worse so that S Sabus and S Meridiani appeared less dark and not brownish but rather bluish in colour.

 

5 July (λ=216Ls) ~ 7 July (λ=217Ls): The dust cloud to the east of Iapygia Viridis showed a vague contour still on 5 July. There were obtained some images by CSr and FMl. According to the images by CPl on 5 July (λ=216Ls) at ω=125W~160W or by ZANOTTI (FZt) on 6 July (λ=216Ls) at ω=143W, there was seen a water condensate near at the morning Ausonia, and so any G and B images were wanted. On 6 July (λ=217Ls), DPk produced the images at ω=219W~238W, DBt at ω=237W, and EGf at ω=249W: The streak of water vapour at the southern M Cimmerium had been weaker. The yellow cloud at Iapygia expanded to Hellas, and concealed the faint M Hadriacum. Here we compare the situation on 6 July by DPk and the later one by Ak on 15 July (λ=222Ls) at ω=235W when the dust was settled. On 7 July, the eastern dust part looked weak, just remaining a bit at Eridania, and the western part was linked with the Noachis cloud (since 6 July). The drawing by WARELL (JWr) at Arizona on 7 July (λ=217Ls) at ω=243W was made from a good angle.

The Noachis cloud showed a new revolution from 5 July. First on 4 July, the dust cloud bent down to the north cutting S Sabus, while on 5 July S Sabus recovered and the cloud bent up to Noachis. The diurnal presence of the dust up to 7 July was summarised in CMO News #3 sent on 8 July as follows: "As far as we caught the first light of a new core of dust disturbance on 4 July from our side (not detected on 3 July), it was furious enough to conceal the eastern part of S Sabus, and looked to possibly make an extension to the northern hemisphere as in 2001, but turned out not. On the following 5th day, the front was rebuilt in the western Noachis with a clear boundary, and looked to swirl back to the direction of Hellas. The assumed Yaonis Fretum and Hellespontus were nothing but two faded blurred spots inside the yellow cloud on the day. S Sabus already recovered its original shape though the eastern tail-end was not so extended southward because the area of M Ionium was cut by a bright band of dust, and rather connected with Syrtis Mj which was dark but going away. On 6 July, the dark band of Hellespontus almost recovered (the northern end was cut out), and the brighter core of dust in Noachis looked slightly shrunk, but yet it had a fat roundish core and we could expect much of this Falstaff to do something. On 7 July, however, he reappeared to have been emaciated within a day, though the wide Hellespontus again looked cut off its head as well as foot by dust, and the slimmed core lay down along the ghosted Hellespontus. Its north-western edge was bounded by a narrow band from Deucalionis R where a branch of dust was seen. S Sabus was normal (no more in chocolate tinge), and the desert adjacent to it looked still reddish. The brighter slimmed core is reminiscent of the cudgel-like dust emergence seen in 1956 starting from Iapygia Viridis straightforwardly to Noachis, but we are not sure this humble Falstaff is vigorous enough to encircle the southern hemisphere up to the south pole."

 Comparison can be made on a chart (click there for a larger .jpg file) made by Mn. Original raw drawings of the dust storm are cited from Mns drawing book and can also be referred (5 July, 6 July, 7 July, 8 July). The various aspects of the dust cloud on 5, 6, and 7 July were ccd imaged though not enough: On 5 July, KPa in Hong-Kong took two images at ω=352W (17:17GMT), and at 004W. On 6 July, MORITA (Mo) at Hiroshima obtained a set of images at ω=338W, Wk at Okinawa at ω=008W, and also ENg in Hong-Kong at ω=010W, WTn in Singapore at ω=021W. On 7 July, ENg caught a just-sinking cloud at ω=005W. During the days, the Noachis cloud showed a large cloud sea connected with the upper cloud over Hellas, and the shadowy markings inside the cloud near at Hellespontus changed every day, as to whose shapes My described later as disgusting.

We are going to make a more detailed review of the Noachis cloud later after the season.

 

8 July (λ=218Ls): The reproduction ability of the Noachis cloud on 8 July looked much weaker. The western border of the cloudy area was measured on 6 July by Id and Mn to be at 340W~345W and since then no further lateral development. On 8 July, the area of M Serpentis turned to appear very changed and looked quite broad and dark. Yaonis Fr was well recovered. Inside Hellas, a shadowy streak was seen from S to N: This is also visible in DMrs images on 8 July (λ=218Ls) at good angles ω=230W~252W. These are preceded by the images by EGf at ω=208W~212W, and followed by MVls images at ω=318W, 348W. Drawings by Mn were made eight times at ω=298W~006W.

On the same 8 July, there was also observed dust lower clouds around near Xanthe. The images by WTn at ω=008W shows them to the east of Nilokeras and at Eos. These places look to apt to keep the condition to generate the disturbances at this season. Earlier ENgs image at ω=342W, and MVls one at ω=348W also show them.

 

9 July (λ=218Ls) ~ 15 July (λ=222Ls): On 9 July (λ=218Ls), the cloud at Noachis, though still scattered yellow cores were seen, could be said to have quite dissipated. Mn visually watched from ω=289W to 357W. By ccd, ENg shot at ω=323W, Wk at ω=330W, 340W, 350W, 359W, and As at ω=340W. On 10 July (λ=219Ls), Mn observed at ω=279W~348W, Km at ω=282W, 292W, 300W, 316W, 320W, 327W, Mo at ω=294W, 314W, and Wk at ω=346W, 350W. On 11 July (λ=319Ls), Mn watched from ω=270W to 338W. On 12 July (λ=220Ls), there were obtained images by ENg at ω=299W at Hong-Kong, and by Wk at ω=303W, 307W, 312W, 317W at Okinawa. Mn watched from ω=261W to 319W. On 13 July (λ=221Ls), ENg shot at ω=281W, and at 317W. Mn observed from ω=251W to 320W. On 14 July (λ=222Ls), EVl obtained images at ω=263W, 280W, Wk at ω=285W, 303W, and ENg at ω=294W. Mn watched from ω=242W to 301W. As seen from the comparison of ENgs image with Kms on 10 July at ω=292W, or comparison of Wks images on 14 July with his on 12 July at ω=303W, we should say not so much difference was made during these days, and the markings look rather fixed with the upward airborne dusts. The images were so rather not clear because of the less transparent atmosphere. On 15 July (λ=222Ls), Ak obtained images from ω=233W to 279W, As from ω=262W to 291W, Km at ω=267W, and 273W, ENg at ω=287W, and WTn at ω=294W, 299W. Mn observed from ω=243W to 291W. As shown by the images of Ak, As, and Km, Hellas was a bit brighter than Ausonia and Trinacria, and M Hadriacum recovered. Judging from the images on 11 July (λ=219Ls) of EGf at ω=203W, and of DMr at ω=212W, the eastern dust looks to have ceased to expand. On this side the original dark markings (ever since the 2001 later period) were not affected, suggesting that the eastern side dust disturbance had been quite milder. Finally, on 15 July (λ=222Ls), PLz noticed that Achillis Pons was again explicit because of a yellow streak at ω=044W. However, according to PLz (see LtE), an IR image taken just after the securing of the RRGB images did not show the streak. So this might suggest something about the ingredients of the yellow streak of this kind seen often at this area. If an R and IR images give different images, the ToUcam images should be more carefully treated.

 WTns newly processed RGB image on 15 July (λ=222Ls) at ω=299W well shows that the higher atmosphere of the planet has been globally yellow hazed because of the preceding dust events.

 

Expansion of Mare Serpentis: As mentioned, by 8 July (λ=218Ls), it became apparent that the area around M Serpentis largely changed and turned to show up as a wide dark marking since the dust which lay before had been swept away or blown up by the furious dust plume storm which occurred on 4 July (λ=215Ls) and so on. See for example MVls ccd images on 8 July from ω=318W to 348W. Here we shall make two comparisons: 1) DPks R image on 24 June (λ=209Ls) at ω=331W with Wks image on 9 July (λ=218Ls) at ω=330W, 2) EGfs on 28 June (λ=211Ls) at ω=302W with Wks on 12 July (λ=220Ls) at ω=303W. These prove a really big change of the area though the latter cases look less transparent because of the rich airborne dust. Needles to say, this is the area worthy of attention in the future.

 

 Inside the SPC: Rima Australis: A clear appearance at this season of Magna Depressio and Rima Australis was given by EGf on 3 July (λ=215Ls) at ω=261W. See also the spc on DPks good images at ω=256W. From the Orient, following images show details: ENgs on 12 July (λ=220Ls) at ω=299W, on 14 July (λ=222Ls) at ω=294W. On 15 July (λ=222Ls), Km gave good image at ω=267W, ENg at ω=287W, and WTn at ω=294W.

Novus Mons: The area is best shown on WTns image taken on 15 July (λ=222Ls) at ω=294W.

Argenteus Mons: This has been bright shown on the edge of the spc from 1 July (λ=214Ls) (eg Mos ω=031W) to 15 July (λ=222Ls) (eg SKws images at ω=026W~ω=050W). This looks to consist of two bright spots, as shown on Kms image on 2 July (λ=214Ls) at ω=023W, and also on the LRGB image of ENg on 5 July (λ=216Ls) at ω=037W. It is detailed also on PLzs image on 15 July (λ=222Ls) at ω=044W.

Parva Depressio: The tadpole inside the spc, mentioned in a previous report, was still seen inside the spc as shot by CPl on 5 July (λ=216Ls) at ω=123W (cf a previous image made by MVl on 24 June (λ=209Ls) at ω=127W). It is also visible on CPls images on 6 July (λ=216Ls) at ω=109W, and BALDONI (PBl)s ω=112W. As Parva Depr comes to the meridian, it becomes a central bigger umbra as seen on CPls images on 3 July (λ=214Ls) at ω=168W & 174W. A detailed description was made by EGf on 13 July (λ=221Ls) at ω=159W.

Another New Mons?: It should be noted that the image of CPl on 6 July (λ=216Ls) at ω=109W also shows a bright spot inside the spc at the tail end of the tadpole, and this is caught clearly also on PLzs image on 8 July (λ=217Ls) at ω=109W. PLzs images in fact caught this bright spot more or less from 7 July to 15 July. Since it is clear on PLzs images on 15 July (λ=222Ls) at ω=044W as well as on 11 July (λ=219Ls) ω=086W, and so this spot is near the south pole, and must be located between pole and Magna Depr. Maybe no sign on ANTONIADIs map.

 

Spontaneous Projection from the SPC: On 4 July (λ=215Ls), on the day the dust storm occurred at the eastern area of Deucalionis R, the present writer noticed a projection downward from the edge of the spc after 17 hrs GMT. It was not seen before. At 17:30 GMT (ω=355W) it was very evident, and remained bright until it went into the night area. Its location was to the east of Argenteus Mons and looked to be situated at the top of Novus Mons. Since it was concealed when ω=044W, it must have been located at around Ω=330W. We hear Id also observed it visually. The brightness was superior to Mons Argenteus. It did not reappear on 5 July.

 

Arsia White Cloud and Dark Olympus Mons: The condensate roll cloud over Arsia Mons was well caught on CPls images on 3 July (λ=214Ls) at ω=170W, on 5 July (λ=216Ls) at ω=160W, and on 6 July (λ=216Ls) at ω=131W and so on. FZts images on 6 July (λ=216Ls) at ω=143W also show it. At this phase angle, it was near the terminator at around ω=170W. CPls images on 6 July show Olympus Mons inside. DPks B images on 13 July (λ=221Ls) at ω=148W, 157W also show the white Arsia cloud, as well as Olympus Mons which appear as a dark spot. Olympus Mons is also evident on EGfs image on the same day at ω=159W.

 

Around Solis Lacus: From the end of June, the area around Solis L was observed from Asia-Oceania region, and then it went to Europe. On 1 July (λ=213Ls), Mn observed until ω=057W (19:10GMT), and then KPa took a ccd image at ω=069W, and ENg at ω=070W (20:00GMT). There was a light spot at Thaumasia Flix to the south of Solis L. The eastern boundary of Thaumasia Flix was bordered with a darkened fringe. Aurea Chersonesus was still light featured. In Europe, the area came into sight from 11 July (λ=219Ls, δ18.4"): KOWOLLIK (SKw) took pictures from ω=054W to ω=083W every twenty minutes. SIEGEL (ESg) started from the day, and impressively saw Solis L at ω=070W. CPl obtained images at ω=062W~077W, and PLz at ω=086W. Claritas looks bright. On 12 July (λ=220Ls), CPl took images at ω=064W~087W, PBl at ω=065W, and PLz at ω=074W. FRASSATI (MFr) observed visually on 13 July (λ=220Ls) at ω=076W. PLzs image of Aurea Cherso made on 15 July (λ=222Ls) at ω=044W is good. GRAHAM (DGh) in England started his observations (colour drawings) from 15 July (λ=222Ls) at ω=059W.

 

Argyre: As the apparent diameter increased, Argyres shape and scale become more apparent. It looked larger, but not so light. Mos images on 1 July (λ=213Ls) at ω=031W, 040W, 049W, 050W show Argyre. ENgs image on 2 July (λ=214Ls) at ω=059W shows more clearly. In Europe, CPls images at ω=038W~040W, and PLzs at ω=057W both on 13 July (λ=220Ls) show well Argyre. ESg began to see Argyre from 11 July, and captured it near the CM on 15 July (λ=222Ls) at ω=028W. The contour was made of double structured: The centre might be the basin. On 15 July, PLz also showed it at ω=044W, and Jesus SANCHEZ (JSc) at ω=058W.

 

M Cimmerium: Details of M Cimmerium were clearly shown on EGfs images on 8 July (λ=218Ls) at ω=208W, 212W. See also DPks images on the same day at ω=197W, 202W. Difference of images may depend on how the dirty atmosphere was processed. The appearance of M Cimmerium is quite reminiscent of what it was in 1988. To the south of the region of M Cimmerium and M Sirenum, there were seen two light round spots: they do not seem to correspond to craters, but will be discussed later after the season.

 

 Around M Sirenum: M Sirenum became to be shot detailed: The images on 13 July (λ=221Ls) of DPk at ω=148W&157W, and of EGf at ω=159W show some GMS particulars while those details on EGfs images look to be given highly enhanced. A dark crater named Caralis Fons is clearly shown. (Note the west end of M Sirenum remains still cut off.)

 

 Elysium and Trivium Charontis: DPks images on 8 July (λ=216Ls) at ω=202W turn to show some details inside Elysium. Trivium Charontis is a dark spot, and Cerberus is shown to have been washed to a weaker spot. The dark patch in theria is of the new shape, as noted before. The inside of Elysium is more explicit on the enhanced image by EGf made on 11 July (λ=219Ls) at ω=203W. The darkness of Trivium Charontis looks very distinguished.

Hi-Fi Images This Period: We recommend best the images of CPl made on 6 July (λ=216Ls) at ω=109W146W because of his descriptions of the spc, white roll clouds, Olympus Mons, and M Sirenum in addition to his image processing of describing the higher atmosphere which has been made impure because of the preceding dust storm (especially the last set of images when the planet was higher up at the latitude of 29 - note his location is nearly 48N, quite northern compared with any Japanese location). PLzs images on 15 July (λ=222Ls) at ω=044W are also fantastic. We should say we also like the gradation shown on EGfs image on 6 July (λ=217Ls) at ω=249W.

 

 


The next issue shall treat the observations made in the second half of July 2003 from 16 July (λ=222Ls, δ19.2") to 31 July 2003 (λ=232Ls, δ=22.2")..


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