th Report:

The CMO/OAA Observations made during a fortnight period from


1 August 2003 (232Ls) to 15 August 2003 (242Ls)


An OAA Mars Section article to be published in CMO #277 (25 August 2003 issue)

Masatsugu MINAMI, Director of the OAA Mars Section

Japanese version here


ow August came in, and the long-expected moment of the closest approach is around the corner. The apparent diameter we experienced this month would never visit until 2018. On 1 August 2003 the angular diameter was δ=22.4", and on 15 August it increased to δ=24.4". The Martian season proceeded from λ=232Ls to 242Ls during this period, and we thus met a very rare season when the centre of the spc began to deviate from the south pole. It was also the season for us to expect that Novus Mons was also detached from the spc. The central latitude φ was 20S/19S, and the phase angle ι decreased from 23 to 13. The Martian altitude at meridian was low from our side since the apparent declination was 13.5S14.5S.

It was said the long-standing rainy season ended over the Japan islands at the beginning of August, but few decisive observations were continuously obtained. At Okinawa, which was free from the rainy season from the end of June, we unfortunately suffered from the passing Typhoon No 10 on 6 and 7 August. If observed, the planet showed increasing details from day to day.



List of 70 Observers

Introductory Notes

Dust at Capri Cornu

The SPC and Its Vicinity

1)   Novus Mons

2)   Bright Spots Surrounding the SPC

3)   Deviation of the SPC Centre

4)   Parva Depressio

5)   Ice Projections

Wine-Coloured Ground



M Cimmerium

The theria Dark Patch

Arsia White Cloud and Olympus Mons


Impressive Images

Observations of the Martian Flares

At Naha


MOUNT of 70 observers contributed. Even then some expected observers were absent: TAN (WTn) and NG (ENg) did not report because they attended the ALPO Meetings invited by Tom DOBBINS (TDb) at Ohio. Even PARKER (DPk) and GRAFTON (EGf) were also kept away for several pressing days. In Europe they were relatively active; we heard however less from LAZZAROTTI (PLz).


AKUTSU, Tomio (Ak) Tochigi, Japan

21 Sets of CCD Images (2, 3, 7, 10 August 2003)

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

ASADA, Tadashi (As) Munakata, Fukuoka, Japan

14 CCD Images (1, 2, 3, 5 August 2003)

30cm SCT with a Panasonic NV-MX5000

BALDONI, Paolo (PBl) Genova, Italia

6 CCD images (3, 9, 10*, 11 August 2003)

18cm Intes-Micro Gold F6, *30 cm SCT with a ToUcam


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

5 CCD Images (1, 3, 8, 11, 15 August 2003)

f/28,3225cm spec with a ToUcam Pro

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

8 Drawings (2,~6, 12, 13, 15 August 2003)

350, 390, 520, 104541cm F/6.9 spec

BIVER, Nicolas (NBv) Versailles, France

2 Colour Drawings (9, 12 August 2003)

51026cm speculum


BUDA, Stefan (SBd) Melbourne, Australia

4 CCD Images (2, 5, 9, 15 August 2003)

25cm and 40cm Dall-Kirkhams with an evolved TC211/TL211

BUNGE, Robert (RBg) Bowie, MD, USA

3 Drawings (7, 12, 15 August 2003)

260, 480, 68043cm F/7.8 speculum

CAPARRS, Angel (ACp) Mlaga, Espaa

3 CCD Image (9, 10, 15 August 2003)

25cm spec with a ToUcam

CARLOS CASADO, Juan (JCs) Figueres, Espaa

4 CCD Images (5, 6, 7, 10 August 2003)

f3615cm spec with a ToUcam

CHAIKIN, Andrew (ACk) nr Boston, MA, USA

1 CCD Image (4 August 2003) 28cm SCT with a ToUcam

CHAVEZ, Rolando (RCv) Powder Springs, GA, USA

3 CCD Images (9, 10*, 15 August 2003)

24cm SCT, *32cm F/6 spec (Cave Astrola) with a ToUcam

COLVILLE, Brian (BCl) Ontario, Canada

6 CCD images (2, 5, 13 August 2003)

30 cm SCT with a ToUcam Pro

COOPER, Jamie (JCp) Northampton, UK

4 CCD Images (2, 4, 10, 15 August 2003)

f/30, 2418cm Intes-Micro Mak-N with ToUcam


CRUSSAIRE, Daniel (DCr) Champigny-sur-Marne, France

6 Sets of CCD Images (1, 2*, 6, 12 August 2003)

10cm Fluorite L with a Vesta Pro

*100cm T with Sony DCR VX2000E at Meudon

DIJON, Jean (JDj) Sillans, Isre, France

4 CCD Images (4, 12/13 August 2003)

f/2750cm spec with a KAF400 chip camera

FRASSATI, Mario (MFr) Crescentino (VC), Italia

4 Drawings (1, 5, 9, 15 August 2003) 250, 40020cm SCT

FUMEGA UCHA, Camilo (CFm) Ourense, Espaa

4 CCD Images (1, 7, 10, 12 August 2003)

f/2531cm spec with a ToUcam

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

3 Sets of CCD Images (1, 2, 11 August 2003)

f/27, 3935cm SCT with an ST-5C

GRAHAM, David L (DGh) North Yorkshire, UK

1 Colour Drawing+1 Note* (2*, 3 August 2003)

16015cm F/15 Maksutov-Cass

HARADA, Yasuhide (Hd) Nagasaki, Japan

3 CCD Images (9 August 2003)

15cm Zeiss refr/70cm Zeiss RC* with a ToUcam

*Nagasaki City Science Museum

HANON, David (DHn) Ringgold, GA, USA

2 CCD Images (2, 9 August 2003)

18cm refractor/41 cm speculum with Sony VX-2000

HEATH, Alan W (AHt) Nottingham, UK

8 Drawings (2, 3, 4, 9/10, 14, 15 August 2003)

200, 28025cm spec/ 20cm SCT

HILL, Harold (HHl) Lancashire, UK

2 Colour Drawings (9, 14 August 2003)

270, 29014cm Maksutov-Cassegrain

ISHIBASHI, Tsutomu (Is) Sagamihara, Kanagawa, Japan

13 Set of B&W and Colour Photos (2, 3, 4, 6, 7, 10 August 2003)

31cm F/6.4 speculum; FCP400F, NP400P (B390)

IWASAKI, Tohru (Iw) Naha, Okinawa Fukuoka, Japan

      22 Drawings (1+, 2++, 12 August 2003) 40021cm speculum

+400, 53031cm spec, 41521cm spec chez ISHADOH,

++43035cmSCT chez TABATA; 53025cm F/8.5spec chez Mn

KARRER, Michael (MKr) St Radegund, sterreich

2 CCD Images (10, 12 August 2003) 18cm Meade Refraktor with a ToUcam

KOVACEVIC, Zlatko F (ZKv) & Robert ZIBREG Virovitica, Croatia

2 CCD Images (4, 11 August 2003) f/20, 4720cm SCT with a ToUcam


KOWOLLIK, Silvia (SKw) Stuttgart, Deutchland

59 CCD Images (1, 2, 5, 7, 8, 8/9, 9/10, 11, 11/12, 12 August 2003)

18cm Starfire Refraktor with a ToUcam Pro

KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan 

19 CCD Images (2, ~6, 10, 12, 15 August 2003)

f/8420cm Dall-Kirkham with a ToUcam

LAU, Canon (CLa) Hong-Kong

1 CCD Image (9 August 2003) f/5935cm SCT with a ToUcam


LAU, Patrick (PLa) Hong-Kong

2 Drawings (9, 10 August 2003) 300, 34025cm Dobsonian

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

4 Sets of CCD Images (10, 12, 13 August 2003)

       20cm F/6 spec/25cm F/5 spec/23cm SCT with KC381, Vesta, ToUcam


LORENZ, Johachim (JLr) Hormersdorf, Deutchland

1 CCD Image (1 August 2003)

f/2530cm spec with a Philips ToUcam

MATSUMOTO, Tatsujiro (TMt) Amagasaki, Hyogo, Japan

1 Drawing and 2 CCD Images (15 August 2003)

60028cm SCT & 54018cm refractor,

28cm SCT with a Sony TRV 900

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

  1 Red CCD Image (14 August 2003)

20cm SCT with a Starlight Xpress MX5

MINAMI, Masatsugu (Mn) Naha, Okinawa, Japan

86 Drawings (1+, 2++ , 3, 4, 5*, 8*, 9,~15 August 2003)

420, 530, 55025cm F/8.5 speculum, * 28025cm SCT

+400, 53031cm spec, 41521cm spec chez ISHADOH,

++43035cmSCT chez TABATA

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

4 Sets of CCD Images (3, 5, 9 August 2003)

f/5025cm speculum with a ToUcam Pro

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

4 Sets of CCD Images (1, 2, 12 August 2003)

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

MURAKAMI, Masami (Mk) Yokohama, Kanagawa, Japan

      19 Drawings (2*, 3*, 6 August 2003) *35015 cm spec, 40020cm spec

NAKAJIMA, Takashi (Nj) Fukui, Fukui, Japan

8 Drawings (2, 10 August 2003) 40020cm ED Goto refractor*

*Fukui City Observatory, Fukui

NARITA, Hiroshi (Nr) Kawasaki, Kanagawa, Japan

9 Drawings (2, 3, 4, 6, 7, 10 August 2003) 40020cm refractor


NIKOLAI, Andr (ANk) Weil der Stadt, Deutchland

2 CCD Image (2 August 2003) 18cm Refraktor with ToUcam Pro

OKANO, Kunihiko (Ok) Setagaya, Tokyo, Japan 

2 Sets of CCD Images (2, 7 August 2003)

31cm F/5 spec with an ST-7XME

OSA, Kanehiro (Oa) Ishikawa, Japan 

1 CCD Image (3 August 2003) 15cm spec with a COOLPIX990

PACE, Ben (BPc) Darwin, Australia

3 CCD Images (1, 7, 9 August 2003)

f/3415cm Maksutov with a ToUcam

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

6 Sets of CCD Images (12, 13 August 2003)

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

PARKER, Timothy J (TPk) LA, CA, USA

1 CCD Image (5 August 2003)

31cm F/22.6 Cassegrain with a ToUcam

PEACH, Damian A (DPc) Herts, UK

1 CCD Image (2 August 2003) f/3220cm spec with a ToUcam


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

14 Sets of CCD Images (1, 4, 6, 9, 11, 13 August 2003)

18cm Newtonian with a modified B&W ToUcam Pro

QUARRA SACCO, Giovanni A (GQr) Valmontone, Italia

2 CCD Images (15 August 2003)

f/4813cm Starfire refractor with a ToUcam

RODRGUEZ RAMREZ, Francisco A (FRd) Gran Canaria, Canary Islands, Espaa

1 CCD Image (15 August 2003) 20cm SCT with a ToUcam

SNCHEZ, Jess R (JSc) Crdova, Espaa

11 CCD Images (1, 4, 9, 10, 15 August 2003)

f/40,4528cm SCT with a ToUcam

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

3 Drawings (4, 14, 15 August 2003) 23010cm refractor

SCHULZ, Robert (RSz) Wien, sterreich

1 CCD Image (3 August 2003) 31cm spec with a ToUcam

SEIP, Stefan (SSp) Stuttgart, Deutchland

2 CCD Images (2 August 2003)

f/3225cm Mak-Cass/f/4316cm Starfire with a ToUcam 740k

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

23 CCD images (1, 4, 6, ~12, 14, 15 August 2003)

41 cm SCT with a ToUcam Pro

SIEGEL, Elisabeth (ESg) Malling, Danmark

9 Drawings (1, 3, 4, 5, 7, 7/8, 8, 9, 10 August 2003)

27020cm F/10 SCT

STGER, Jrgen (JSt) Katzelsdorf, sterreich

1 CCD Image (10 August 2003) f/4010cm Refraktor with a ToUcam

SURO, Jos (JSr) Tierra Verde, FL, USA

2 CCD images (3, 12 August 2003) 28cm SCT with an Olympus C4000Z

TATUM, Randy (RTm) Richmond, VA, USA

2 CCD Images (14, 15 August 2003) 25 cm spec with a ToUcam

TEICHERT, Grard (GTc) Hattstatt, France

6 Drawings (2, 3, 5, 7, 9, 13 August 2003) 33028cm SCT

TSUNEMACHI, Hitomi (Ts) Naha, Okinawa, Japan

34 Drawings (11, 12, 13, 15 August 2003)

530, 55025cm F/8.5 speculum


VALIMBERTI, Maurice P (MVl) Melbourne, Australia

8 CCD Images (1, 2, 5, 9, 15 August 2003)

f/3435cm SCT with a Philips ToUcam Pro


Van Der VELDEN, Erwin (EVl) Brisbane, Australia

4 CCD Images (10, 12, 13 August 2003)

f/3120cm SCT with a Vesta Pro modified


WALLER, Skip (SWl) Dallas, TX, USA

2 CCD Images (8, 10 August 2003)

f/5025cm SCT (LX200) with a ToUcam Pro

WARELL, Johan (JWr) Tucson, AZ, USA

       3 Drawings (5, 6, 10 August 2003) 26025cm SCT (LX200)

1 CCD Image (10 August 2003) f/2325cm SCT with a ToUcam


WIENECKE, Marcus (MWn) Frndenberg, Deutchland

2 CCD Image (9, 15 August 2003)

f/2025cm SCT (LX200) with a ToUcam Pro


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

3 Sets of CCD Images (1, 10 August 2003)

f/4520cm spec with a Philips ToUcam

ZANOTTI, Ferruccio (FZt) Ostellato (FE)/*Forca Canapine (PG), Italia

2 Sets of CCD Images (3, 11* August 2003)

45cm spec/*24cm SCT with a ToUcam                



ntroductory Notes: The angular diameter of Mars exceeded 22 arcsecs, and the details of markings were becoming more apparent every day than expected for the less-experienced observers, while the most experienced observers were feeling that the Martian atmosphere has looked quite dirty. At Okinawa, ISHADOH (Id) complained every time the surface was quite dusty: This must have been caused by the fallout of dust in 2001/2002 and the recent rise of airborne dust. As we heard, Harold HILL (HHl) in England started from 25 June 2003 and observed in August on 3, 4, 6, 9, 10, 11, 13, 14, 16th days, but he stated that the planet in August was more yellowish to his naked eye rather than ruddy. ISHIBASHI (Is) remarked in the Observing Note of his images on 2 August from 17:20 GMT (ω=094W) to 18:27 (ω=111W) that the dark markings looked fainter in contrast with the spc brightness, and quite different from the darkness seen even in mid-July (in LtE #276). Is also reported an episode that he had gotten on the phone from Reiichi KONNAI (n HORIGUCHI) who has been a comrade of Is and once produced superb Martian images (TriX and fine drawings) at the beginning of August 1971 around λ=225Ls (he obtained also excellent results about the Solis L dust storm in 1973): KONNAI recollected and assured that this years dark markings looked fainter, while in 1971 (before the rise of 1971b) the surface markings were complexioned quite darker. The 1971b dust started around on λ=260Ls, while the first 1971a occurred at the same season as the 2003 Deucalionis Dust entrained in July. In the Viking year, the first dust storm rose at λ=205Ls, and the optical depth τ increased from 0.5 to 3, and after a moment diffusion, the depth increased upto τ=4 because of the rise of second dust at λ=268Ls. The atmospheric pressure increased rather linearly from λ=180Ls to λ=270Ls: This might have been due to the sublimation release of CO2 from the spc while the airborne dust must have contributed. According to a model by C E NEWMAN et al (JGR 107 (2002)), the optical depth really increase from 1 to nearly to 5 in the period from λ=180Ls to λ=270Ls. As to the yellow colour, which is especially more evident near the limb side, E SIEGEL (ESg) described about the morning limb at the southern continent as not bright but showing a colour of deep yellow like old butter at ω=145W on 7 August (λ=237Ls) through IL (not visible in Wr#25). This must have been related with a temporary thicker veil, but ESg reported it was not visible next night at ω=137W.

 From Asia and Oceania, the regions from Solis L to Syrtis Mj were observable during the present period, and from Europe they observed the regions from M Cimmerium to Solis L, while the region of S Sabaeus to that of M Sirenum faced to the US.


Dust at Capri Cornu: The dust streak which appeared on 29 July (λ=231Ls) at Achillis Pons looked to cause another rise of dust at Chryse on 30 July (λ=231Ls) whose early morning state was well observed in the US. On 31 July (λ=232Ls) the remainder came to be observed in Asia and Oceania, and a weak rise of core was checked at Eos (by chance several images at ω=069W by BAd, MVl, Km, and As). The Eos dust was already observed at America and witnessed also at Xanthe along the contour line. Eos must be a concave area, and the area to raise a every day dust devil.

On 1 Aug (λ=232Ls), from the morning time, in addition to the Eos dust, there was seen a dull yellow cloud over Pyrrhae Regio as well as another dust toward Protei R as shown on the images of GRAFTON (EGf) at ω=342W, BATES (DBt) at ω=345W, WILLIAMSON (TWs) at ω=351W, SHERROD (CSr) at ω=353W, and of TWs at ω=002W. TWss images are separated by 40 minutes and may provide more accurate variable situation. A faint yellow cloud must also have been flowed down to the Oxia Palus area. Note however the bright Aram is not because of the dust. As the planet rotated to Oceania and Asia, VALIMBERTI (MVl) made an important shot at ω=060W. Successively, MORITA (Mo) took at ω=073W, and PACE (BPc) at ω=081W. ASADA (As)s image at ω=104W also shows a bit. At Okinawa, the sky was fine and ISHADOH (Id), IWASAKI (Iw) and the present writer (Mn) watched the dust disturbance chez Ishadoh. Iw was there to join the watching team of the possible flares at the Solis L region (as described below). The visual observation first was made by Mn at ω=057W, while the planet was still low. Iw first checked the dust at Eos from ω=062W, and then watched at ω=072W, 082W, (and thus every 40 minutes ten times until ω=149W at 20:15 GMT (quite dawn). The dust was seen from Eos to Pyrrhae R, and it was brighter than Argyre. It was concealed however from the terminator at around ω=101W.

 On 2 Aug (λ=233Ls), the dust was rather conspicuous at Capri Cornu. EGfs image at ω=328W is important in the sense it captured an early rise of a bright dust at Capri Cornu. After the Pacific Ocean gap, MVl took it near the CM at ω=034W. And then an excellent series of images was produced by AKUTSU (Ak) at ω=037W, 047W, 056W, 066W, 076W, 088W, 097W, and 106W (eight images!). The dust from Eos to Capri Cornu is clearly shown there. The images are stable from ω=056W, or 066W, and also show an extension of dust over Pyrrhae R. BUDA (SBd)s image at ω=042W is also suggestive. KUMAMORI (Km) took at ω=049W and 061W, and ASADA (As) also took successively at ω=051W, 062W, 070W, 080W, 089W, 099W, 110W: The images are stable around from ω=070W. MORITA (Mo) took at ω=065W. At Okinawa, we were to kill two birds with one stone: We were gathering at Tabatas Observatory to check the flare, and at the same time Iw and Mn were prepared to check the dust by a 35cm SCT. The seeing condition was good from the early evening, and started from 13:30 GMT at ω=038W. AKUTSU (Ak) already started the day from 13:24 GMT, and so he was earlier, while our longitude at Naha is behind the longitude of Nasu where Ak stays by 12 or by 50 minutes, and so we should say we started from the lower Mars. Iw and Mn then alternatively observed at ω=043W(Iw), 048W(Mn), 053W(Iw), 058W(Mn), 063W(Iw), 068W(Mn), 073W(Iw), 077W(Mn), 082W(Iw), 087W(Mn), 092W(Iw). Then we moved to MINAMIs observing site and observed until ω=136W(Mn), 140W(Iw; 20:25GMT) to check the shadowy area inside the spc. To our eyes, the dust expansion to Pyrrhae R was clear and the lower staying dust at Capri Cornu looked cudgel-like or it was literally horn-like, and apparent near the terminator until ω=090W. We should say however the brightness did not suggest any of the big dust.

3 Aug (λ=234Ls), no other observation of dust was made than in Asia. Ak took a series of images at ω=028W, 036W, 046W, 056W, 071W, and 080W. It is quite noteworthy that these were made at the same angles as the day before. The direct comparison easily shows that the dust at Capri Cornu has weakened and another branch looks to have expanded to the direction of Argyre. Mn also observed at ω=029W, 039W, 049W, 059W, 068W, 078W, 098W, 117W, 127W (rain showers twice), and Km took at ω=054W, 072W, 086W. ASADA (As) also shot at ω=065W, 075W, 086W. The dust branch at Pyrrhae R has been weakened. Visually the all over yellow haze looked to have more increased. Notable is that the dust streak at Achillis Pons was still existent; implying there remained still a condition of dust raising as in late July. We should think the dust was not propagating, but the catastrophe condition was fulfilled at each place.

On 4 Aug (λ=235Ls), Mn observed at ω=040W, 050W, 059W, 069W, 079W, 089W, 098W, 108W: The dust was still confined inside Capri Cornu, and dull expansion of thin yellow cloud over Pyrrhae R was seen to the terminator. The images by Km at ω=044W, 080W, 099W well show a bright core inside the dust at Capri Cornu which was apparent even near the terminator. On 5 Aug (λ=235Ls), Typhoon No 10 was approaching and Mn checked the area no more than three times at ω=031W, 041W, 050W. The horn area was seen but the dust was quite dull. On the day, MVl took the ccd images at ω=009W, 025W, SBd at ω=016W, Km at ω=035W, 044W, and As at ω=036W, 047W, 058W: None showed the preceding-days brighter core inside Capri Cornu. On the same day, MOORE (DMr) secured images at ω=319W as well as Tim PARKER (TPk)s at ω=343W, but no early morning activity is seen at Capri Cornu. We miss the images by EGf and DPk on those days.

On 6 and 7 August the present writer (Mn) was blind confined in his resident room during Okinawa was in the Typhoon area, while Km took excellent images at Sakai, Osaka on 6 Aug (λ=236Ls) at ω=074W, 081W. There seems to show a local expansion at the bulge of the bugle. On 7 Aug (λ=236Ls), Ak produced a series at ω=001W, 011W, 021W, 039W, 049W. The area of M Erythraeum was well shot, and the dust expansion is seen over Argyre just like at Pyrrhae R. The dust at the west southern part of Capri Cornu seems also slightly expanded to Protei R. BPc took also at ω=026W, and OKANO (Ok) at ω=032W which all show the region in question. Note that the yellow haze has increased on the surface. On 8 Aug, no explicit observation was obtained concerning this area. On 9 Aug (λ=238Ls), the remaining dust was seen at the low area at Eos and Capri Cornu, while another branch of thin dust was seen to the direction of Deucalionis R and also at Chryse. This is shown on the images by HARADA (Hd) made at ω=004W029W, and otherwise those by MVl at ω=004W, BPc at ω=025W, and Canon LAU (CLa) at ω=049W. From Okinawa, we watched from the angles of ω=355W, 005W, 005W, 024W, 034W, 044W, 053W, and 063W. Achillis Pons was still with a bit of dust, and thus the dust event this time should be motivated in the northern hemisphere. At the end of the present period, we could catch from Okinawa the angles around ω=027W on 13 Aug (λ=240Ls) at 19:30GMT (4:30 JST): Capri Cornu was weak but showed its horn shape with a thin dust inside.

[NB: The nomenclature Capri Cornu was given by E M ANTONIADI. Capri is the genitive of Caper (Goat) and Cornu (Horn) is a nominative, and so Cornu Capri implies a Horn of Goat. ANTONIADI employed monomaniacally several names beginning with C of such star constellations around here as Ceti L, Canis F, Canopi F, Columbae F, Corvi L, while Capri Cornu is the most appropriate to express the horn or cone shape dusty area. This area has been known since SCHIAPARELLI in 1877 and others, but seems to have been neglected by EBISAWA?]


 The SPC and Its Vicinity: 1) Novus Mons: EGfs excellent image on 2 Aug (λ=233Ls) at ω=328W well indicated that Novus Mons had already separated from the spc. See also the magnified figure. BATESs (DBt)s image on 3 Aug (λ=234Ls) at ω=324W also suggests the detachment. See also the images of the spc on MOORE (DMr)s on 3 Aug (λ=234Ls) at ω=329W(R), as well as on TPks on 5 Aug at ω=342W. The season λ=233Ls is identical with the epoch spotted by Mariner 7 (CUTTS, VEVERKA, GOGUEN, Icarus 16 (1972) 528). On the other hand the critical season spotted by the Viking in 1977 was at λ=242Ls. The present writers Observing Note after the Typhoon made on 9 Aug (λ=238Ls) at ω=355W records that Novus Mons had been definitely detached. The season of the detachment of the peninsula as it was first observed in 1845 was said around λ=249Ls by E C SLIPHER. Later observations, including those by LOWELL and BARNARD in 1894, seem to indicate λ=251Ls as a mean value. However, according to ANTONIADIs list, the season by LOWELL and BARNARD in 1894 was around λ=220Ls. The result of ANTONIADI in 1909 implied λ=247Ls, while LYOTs one in 1924 pinned down λ=242Ls. The judgment of the separation must be not so easy partly because it must be difficult to probe the area of the root of Novus Mons. For example, the peninsula is well spiked out on the Viking image of the spc at λ=255Ls, while the root can also be stuck still to the main spc. In this sense, the aspect of the western follower (not rotationally) of Novus Mons is interesting. The following images are suggestive: on 8 Aug (λ=237Ls), WALLER (SWl)s at ω=282W, DBts at ω=297W as well as CHAVEZ (RCv)s image on 10 Aug at ω=249W and DBts image on 11 Aug (λ=239Ls) at ω=231W. The angle of the image of WARELL (JWr) on 10 Aug (λ=238Ls) at ω=277W is good, but the image looks slightly embossed. According to our observations on 15 Aug (λ=242Ls) at around ω=287W, the follower (rotationally preceding) was still remaining, while near the terminator it became very dimmed as recorded on 12 Aug (λ=248Ls) at ω=328W and so on. The aspects at λ=240Ls~242Ls this year were caught by Km, Mo, and EVl on 12 August at ω=346W, ω=353W, and ω=358W respectively, and MVl and SBd on 15 Aug (λ=242Ls) at ω=287W/310W, and at ω=297W respectively. Note that Novus Mons was not uniformly bright, but showed two brighter spots, one at the tip and the other at the halfway belly as recorded on 11 Aug (λ=239Ls) at ω=337W by Mn. These bright spots must have bee made by the reflections of the sunbeam at the water ice masses.

2) Bright Spots Surrounding the SPC: To the west of Novus Mons, Argenteus Mons at around Ω=030W shines with a fine structure (two spots) but did not yet show the big collapse. Mn noticed another small bright point to the slight west of Mons Argenteus on 4 Aug (λ=235Ls) at ω=040W. See Argenteus Mons on the images on 7 Aug (λ=236Ls) at ω=026W by BPc and at ω=032W by OKANO (Ok) as well as on MVls image on 9 Aug (λ=239Ls) at ω=004W, Canon LAU (CLa)s image at ω=049W, Patrick LAU (PLa)s drawing at ω=025W. Further westward, there is a bright spot near Ω=080W to the south of Solis L. See Kms images on 3 Aug (λ=234Ls) at ω=072W, as well as on 4 Aug (λ=235Ls) at ω=080W. Furthermore at around Ω=150W, we meet Thyles Mons. Its shape was depicted on the images by PELLIER (CPl) on 6 Aug (λ=236Ls) at ω=172W, on 9 Aug (λ=237Ls) at ω=140W, as well as on LAZZAROTTI (PLz)s 10 Aug (λ=238Ls) at ω=140W. DPks images on 13 Aug (λ=240Ls) at ω=190W also gives us a clear cut image. See also KARRER (MKr)s on 10 Aug (λ=238Ls) at ω=147W. The peripheral bright spot shown on the drawing by FRASSATI (MFr) on 15 Aug (λ=242Ls) at ω=129W as well as on the image by TATUM (RTm) on ω=170W is Thyles Mons. If seen further west of ω=200W, the contour is made of several light beads including Thyles Collis. For instance, CPls images on 1 Aug (λ=232Ls) at ω=230W and SEIP (SSp)s on 2 Aug (λ=233Ls) at ω=233W show the beads. However ten days after, the eastern part had hastened to thaw and the roundish aspect was broken and showed a corner which was located around at Ω=230W. These can be seen if compared with the periphery of the spc on the images of EGf on 11 Aug (λ=239Ls) at ω=231W as well as on DPks on 12 Aug (λ=240Ls) at ω=231W. Here we cite one from CPls at λ=232Ls and EGfs at λ=239Ls. Also the images by HANON (DHn) on 9 Aug (λ=237Ls) at ω=237W as well as DBts on 11 Aug (λ=239Ls) at ω=238W are also instructive.

3) Deviation of the SPC Centre: As was noticed a precursor in the preceding issue, the deviation of the centre of the spc has begun to move around from λ=230Ls, and so the observation was pressing from 1 August (λ=232Ls). The present writer (Mn) as well as Iw watched up to the angle ω=135W, and noticed that the western side of Thyles Mons had become less bright. On 2 Aug (λ=233Ls) Mn observed with Iw up to ω=136W and obtained similar result though the thawing was inadequate. On 4 Aug (λ=235Ls), we saw the morning side of the spc looked slightly shadowy (partly because of the airborne dust) from ω=050W. Since we thought the season λ=235Ls was critical, we sent out a notice (CMO 2003 News #5 with Subject: Deviation of the centre of the spc from the south pole) from cmo@ on 7 August 2003 at 1:10 GMT. We then readily received the following reply from Elisabeth SIEGEL (ESg) in Denmark: "In response to your e-mail "CMO 2003 News #5" I should like to inform you that as I observed Mars last night (August 7 at 00:10 UT, with an ω of 158.3W), I noticed that the following about-one-fourth of the SPC looked thin and shadowy. I was quite unprepared for this sight (I just read your email, and it is now mid-afternoon here), and the last time I observed - on August 5, also just after midnight UT - I did not notice anything of the kind. So your message was most pertinent, it seems... and right on the mark." ESgs Observing Note on 7 Aug (λ=236Ls) at ω=158W records that the boundary looked sharp. She also made a similar observation one day after at ω=145W (23:50GMT on 7 Aug). KOWOLLIK (SKw) was observing also on 6/7 Aug (λ=236Ls), and her series of ccd images showed that the right-hand side of the spc had been less bright at ω=147W, 156W, and 166W. This aspect is evident and definite also on the images by CPl on 9 Aug (λ=237Ls) at ω=140W(R), 142W(G), by PLz and his comrades on 10 Aug (λ=238Ls) at ω=140W, by MKr at ω=147W, and by PBl at ω=154W (Thyles Mons is made of two bright spots on CPls images). PLzs IR image on the day at ω=114W suggests well how the aspect will appear later from ω=140W.

As stated previously, as the season proceeds to λ=240Ls, the east of Ω=230W becomes shadowy and so we can easily catch the area where the thawing is rapid. DPks images on 13 Aug (λ=240Ls) at ω=190W~204W show the area from Thyles Mons to this point and hence these images will be compared later with the later thawed-away case. RCvs image on 15 Aug (λ=242Ls) at ω=187W, since this being harder processed than DPks, suggests well the area to be thawed away.

If we see the spc from ω=230W to 320W, then the left-hand side of the spc should appear to be more shadowy: The image cited in CMO News #5 was the one made by CHAIKIN (ACk) on 4 Aug (λ=234Ls) ω=281W, and this gives the case in good contrast. DMrs images on 5 Aug (λ=235Ls) at ω=318W also show this. It is also clear on images on 8 Aug (λ=238Ls) by SWl at ω=282W, and by DBt at ω=297W. The angle is slightly shallow, but DHns image on 9 Aug (λ=237Ls) at ω=237W also shows the contrast. The images on 11 Aug (λ=239Ls) by EGf at ω=231W as well as by DBt at ω=238W prove clearly the shadowy area from the far different angles. Finally, on 15 Aug (λ=241Ls), MVls images at ω=287W311W, and SBds at ω=297W show the good images of the spc. Note that the thawed-away area shows a tint of ochre. This may be check on EVls image on 13 Aug (λ=240Ls) at ω=315W, 331W, and also apparent also to the naked eyes at Okinawa.


4) Parva Depressio: This time we have few observations about Parva Depressio which was detailed in a previous issue from the angles ω=123W129W. On 1 Aug (λ=233Ls), Mn caught the area at ω=116W, 126W, 135W (also on 2 Aug at ω=126W and so on), while the tadpole was not conspicuous, and looked to have melted into the shadowy part beyond Thyles Mons which belonged to the rapidly thawing part of the spc. Kms image on 3 Aug (λ=234Ls) at ω=123W shows the deformed area of the tadpole, and CPls images on 13 Aug (λ=240Ls) at ω=123W may show the final stage. MKrs image on 12 Aug at ω=117W is also interesting.


5) Ice Projections or the Cascades: At Okinawa we observed during this period the surfaces from Solis L area to the regions of Syrtis Mj, but in this breadth we have not so much observed the ice projections from the periphery of the spc. Especially Mons Argenteus did not decay. Scarcely, on 4 Aug (λ=235Ls) at ω=050W, the outskirts of Argenteus Mons showed a weak cascade, and on 13 Aug (λ=240Ls) at ω=358W, another cascade was seen to the south of Noachis. On 12 Aug (λ=248Ls) at the ω=328W session, we saw a projection toward north from the outer side of Novus Mons. On 14 Aug (λ=241Ls) at ω=301W, we observed a projection from the top tip of Novus Mons. Maybe the projection-like tip of Novus Mons seen on MVls images on 15 Aug (λ=241Ls) at ω=277W, 310W as well as on SBds image at ω=297W must be non-ghostly.


Wine-Coloured Ground: The Martian surface has apparently been covered by a vast yellow veil of haze made of airborne dust, and the upper atmosphere looks quite dirty, increased the more by the recent dust at Chryse-Eos-Capri Cornu. However the veil of haze appeared not uniform, and we could tell some divergences in colour. On 4 Aug (λ=235Ls) at around ω=040W, 050W, the present writer noticed that the higher latitude region around Argyre to Noachis showed a ruddy tint or wine-colour. We thought that this was because the higher-latitude region was thinner than or rather free from the yellow dust except for the morning and evening sides. This wine-coloured areas sometimes appeared to our eyes, and as another case we noticed the colour at the shadowy area to the south of Hellas to be wine-coloured on 15 Aug (λ=242Ls) at ω=287W~ and this was also confirmed by TSUNEMACHI (Ts) by the same telescope. Even at ω=000W (at 18:50 GMT), the area to the south of Noachis was appearing wine-coloured while its north was largely dirty yellowish.


Hellas: NG (ENg), who was absent for a month staying in the US invited by Tom DOBBINS, left an important series of images before he flied away on 18 July (λ=223Ls) at ω=234W~279W, as was cited previously. These show that the Hellas basin was full of lower sandy-yellowish matter inside at the morning side. MORITA (Mo)s images on 16 July (λ=223Ls) at ω=229W~273W also showed the same phenomenon. This was taken when the phase angle ι=32, while it decreased to ι=10 this time, so that the effect from the upper air must be less. However as shown by the excellent images of CPl on 1 Aug (λ=232Ls) at ω=206W~270W, the expansion of the yellow veil over the morning side is still stronger. Furthermore, different from the ENg and Mo case in July, the cloud looks to show an outflow of dust down to Trinacria, higher on air than in July. This is shown also on WILLIAMSON (TWs)s image made on 10 Aug (λ=238Ls) at ω=256W. EGfs LRGB images on 11 Aug (λ=239Ls) at ω=231W looks different in nuance than the usual image by TWs, but it still shows that the airborne dust stays higher over the morning Hellas.

Evening Hellas is also interesting, while it is rather difficult to observe because the area turns to be dimmer. On 10 Aug (λ=238Ls) at ω=327W, 336W, Mn observed that the area of Hellas looked ruddy in the same way as Aeria, but veiled thin white-yellowish mist, and it proved much dimmer at ω=346W (ι=16).


 Trinacria: As reported previously, the light-shade aspect of Trinacria has been very different from the aspect we saw in 1988, and as the angular diameter increased much, its detail has become more and more apparent. Some ccd images are judged never cool if its description is rough. In this respect, CPls images taken on 1 Aug (λ=232Ls) at ω=228W~267W are excellent despite the use of no more than 18 cm: The assumed dark line which connects M Hadriacum and M Tyrrhenum is shown now how it is composed of small dark spots. They show clearly how M Hadriacum extends, though split and broken, to the east to invade Ausonia Australis, and its branch running to the south looks like a broad doubled canal. Such other images as SWls on 8 Aug (λ=237Ls) at ω=282W, DMrs on 9 Aug (λ=238Ls) at ω=275W, 284W, RCvs and SWls on 10 Aug (λ=238Ls) respectively at ω=249W, and at ω=263W, and DBts on 11 Aug (λ=239Ls) at ω=238W are all show these aspects. Among them, the images by EGf made on 11 Aug (λ=239Ls) at ω=231W show most clearly the details: A fine segment seems to run from the middle point to the dent on the southern coast of M Tyrrhenum (to be compared with MOCs images), and the complex description of the eastern part of M Hadriacum is excellent. DPks images on 12 Aug (λ=240Ls) at ω=234W also show the fine structure of the area. Note these areas will be no longer out of sight from the US until mid-September. Here we choose a TP photo made by Isao MIYAZAKI (My) in 1988 to compare the 1988 aspect of Trinacria with its present status.


M Cimmerium: Contrary to Trinacria, M Cimmerium looks to remain the same as in 1988. When we saw it in 1986, because it was on the upper side because of the difference of φ, we sometimes called its shape as like a water beetle or pond skater with several legs including so-called Cerberus III, while in 1988, we changed to call it as grasshopper-like or something like that (by My and others). One of the features was a conspicuous leg (doubled) which must have been a remnant of S Gomer or corresponding to the classical Sinus Cyclopum which projected northward like a spike. It was rather difficult to discern when the angular diameter δ has been not large. However this time as the δ increased to 22 arcsecs, any observer using a 18cm scopes has begun to catch clearly this grasshopper leg. First KOWOLLIK (SKw) who is using a 18 cm Starfire showed it clearly on 1 Aug (δ=22.4", λ=232Ls) at ω=245W. Her friend NIKOLAI (ANk) also showed it on 2 Aug at ω=219W, 234W. BALDONI (PBl), using a 18cm Mak-Newton showed it on 3 Aug at ω=200W. PELLIER, with a 18cm Newton, not first but also spiked down on 4 Aug (λ=234Ls) at ω=197W, and on 6 Aug (λ=236Ls) at ω=192W in full length. By the use of a 15cm CASADO (JCs) showed it on 5 Aug at ω=191W. Another could-do 18cm Mak-Newton user PLz was not active at the beginning of August, and just his image on 30 July showed the leg, but not near the CM. More detailed aspect of M Cimmerium is also shown on EGfs ccd images on 11 Aug (λ=239Ls) at ω=232W (or above cited). This shows that the leg kicks back a stain, but this image proves that the stain have survived in the same way as in 1988 (refer here to MIYAZAKIs drawing in 1988).


 The Aetheria Dark Patch: Already it was several times noted that the theria dark patch was caused to change its shape due to the dust disturbance around 2 4 July 2001, while its detail has now been more apparent since the apparent diameter increased. See EGfs image on 11 Aug (λ=239Ls) at ω=231W and DPks on 12 Aug (λ=239Ls) at ω=234W and so on.


 Arsia White Cloud and Olympus Mons: This period, few observations were made about the evening Tharsis. CPls images on 9 Aug (λ=237Ls) at ω=140W, 170W show an early afternoon Arsia with explicit white cloud (see B images). It is well known that the orographic cloud at the summit of Arsia Mons is very active during this season. See for example several images by CSr on 15 Aug (λ=241Ls). A critical case was obtained by DPk on 13 Aug (λ=240Ls) at ω=190W, 193W: These prove of course a white Arsia Mons near the terminator, while it also seems to show that the summit of Olympus Mons is also whitish contrary to an established belief. It may be possible that saturation of water vapour may occur when it comes very near the terminator at this season. However no other observations here are known preceding the moment. CSrs image on 15 Aug (λ=241Ls) at ω=187W is also critical and may need a preceding series.


 Others: The vast darkened new area at M Serpentis to Noachis, which was caused by the dust disturbance at Deucalionis R from 4 July 2003, looks to remain still unchanged. The region of Solis L looks also the same as before (detailed): the bright area at Aurea Cherso is quite light as well as Thaumasia Flix




mpressives: One of most impressive files this period is AKUTSUs images which were taken on 2 Aug (λ=233Ls) at ω=037W~106W: Each image is excellent and above all the file consists of a sequence of images especially revealing the trend of the Capri Cornu dust (to be compared with those on 3 Aug). KUMAMORIs Solis L on 6 Aug (λ=236Ls) at ω=074W is also impressive: Note this was taken by the use of a homemade 20cm Dall-Kirkham when δ23.3".


Abroad, PELLIER (CPl)s files are all attractive: especially the file made on 1 Aug (λ=232Ls) at ω=206W~270W is the most impressive. VALIMBERTI (MVl)s image on 9 August (λ=237Ls) at ω=004W was fascinating and at last on 15 Aug (λ=241Ls) he gave a final impression with the images at ω=277W, 310W.


Not to mention, GRAFTON (EGf)s images on 11 Aug and Don PARKER (DPk)s images on 12 Aug gave us extra impressions.





bservations of Martian Flares: (I) The checking of the possible flares on Martian surface has been and is still pressing in 2001, 2003 and 2005 ever since the American team succeeded in confirming the flares at Edom in June 2001. The year 2003 thus proved to provide an opportunity for the Japanese observers to meet with the flare around Solis L as Sanenobu FUKUI observed in 1958. According to MURAKAMI (Mk), the coincidence DE=DS=20.1S was known to occur on 1 Aug 2003 at 23h GMT, and so we prepared to organise teams. The following list was prepared by Mk (15:00 GMT =00:00 JST):


 Rise of Mars Meridian      Rise of the Sun

Altitude 0 15 30      42        30 (at 35N)











29 July






























01 Aug









































Two teams were assumed: one at Naha led by H ISHADOH (Id) and the other at Tokyo led by MURAKAMI (Mk). In Tokyo, the CMO received a proposal from a staff of the National Astronomical Observatory to jointly pursue the phenomenon at the NAO, and some CMO members prepared to join. However this plan was broken because another notorious staff of the NAO was not willing to collaborate: Mk then reorganised another team with the supervisor and members (students and the Old Boys) of the famous Astronomical Club of the Tokyo Kudan High School (Mks alma mater).


T Naha, ISHADOH (Id) and his comrades made a team. They decided to observe about four hours every day from 30 July to 3 August in Naha. On 30 July, we gathered at Ishadohs Observatory. A 25 cm SCT was set on the rooftop to send the live Mars image to a monitor which four persons including WAKUGAWA (Wk) and TABATA (Tb) watched. If they could find something strange on the monitor, they should send a caution to Id and Mn who were near the 31cm and 21cm reflectors on the same roof. Id and Mn were near the telescopes and watching Mars, but not always at the eyepieces, but if a caution came they were to readily catch the Mars surface. We started from after 13h GMT and ended at around 18h GMT on 30 July. However we have not notice any flare phenomenon. We should note that that night the clouds floated frequently, and so the watching was not perfect. On 31 July, we moved to Tabatas Observatory: The Video system was the same as used the day before, and the visual telescopes were a 35cm SCT and a 25cm Schiefschpiegler. We watched from 13:30 to 17:00 GMT. Unfortunately no flare was detected. On 1 August, Tohru IWASAKI (Iw) flied from Fukuoka to Naha to join us. The night we observed on the rooftop of Ishadohs. The Video system with the 25 cm SCT was the same. Seeing was rather good, but no result about the flare was obtained. Even after the flare watching Iw stayed at the Ishadoh Observatory and observed the surface. The photo here was taken at dawn (From left to right: Id, Iw and Ids 31 reflector). On 2 August, we gathered at Tabatas Observatory, and the 25cm SCT + Video system were retained. Iw and Mn used alternatively the 35cm SCT. The night the seeing condition was fair from the time the planet was low, but unfortunately we could not detect any happening concerning the flare phenomenon. We observed otherwise the dust at Capri Cornu. We closed our watching at Tabatas by 17h GMT, and then Iw and Mn moved to Minamis watching roof site (quite near Tabatas) and they observed the inside of the spc by the 25cm reflector. On 3 August, Id and Wk continued to watch the surface to detect flares at Wakugawas Observatory by the use of the 25cm SCT (Video taped) and a 40cm reflector; but it was reported that no flare was observed. Mn stayed at his observation site to do the routine observations the night.

 We had an impression throughout the watching that the surface looked too dirty to detect a delicate fluctuation of flare if any. We were also afraid that the dust fallout in 2001/2002 might have caused a decisive change on the ground around the Solis L region compared with the case in 1958.


URAKAMI (Mk)s team in Tokyo also planned to watch from 30 July to 3 August, while it was cloudy on 30 July and 31 July. Their formation at Kudan was as follows: The main 15cm ED F/15 refractor inside a dome (photo here) was attached with a Sony VX2000 Video Camera to send the planet image to a monitor which about 5 persons watched. Mk and others were near a 15cm reflector to check if any information could come from the monitor team. Mk was to do usual observations. Other OB members used a 20cm Cass (Takahashi CN221) equipped with a ToUcam. On 1 August, still the clouds floated, and just the Video worked no more than one hour from 15h GMT. On 2 August, the sky was slightly better, and the Video worked from 14:55 GMT ω=059W to 19:35 GMT ω=127W; but the condition was not so stable because of the coming and going of clouds. On 3 August, the rainy season ended in the Kwantoh District (including Tokyo, Kanagawa, Tochigi), and they enjoyed a fine sky. The Video worked from 14:25 GMT ω=043W~18:00 GMT ω=095W, and the 15cm telescope was on alert, but no flare was reported. During the session the ToUcam made a set of 11 image files and Mk made twenty minute observations eight times (from 14:20 GMT ω=042W to 19:00 GMT ω=110W). Here we cite a ToUcam image at 15:27GMT with ω=058W. Total of 20 observers joined and ten hours were spent for the Video during the days, while no flare was unfortunately checked.


SHIBASHI (Is), at Sagamihara, Kanagawa, tried to watch the possible flares alone by the use of his favourite 31cm reflector equipped with a Video camera. He could observe on 2 August from 17h GMT to 19h GMT, on 3 August from 15 h to19h GMT, and on 4 August from 14.5h GMT to 16h, but he also did not detect any flare.


(II): Tatsujiro MATSUMOTO (TMt) at Mukogawa near Kob, Hyogo Prefecture, detected a white flare near the Huygens crater on 15 August at around 15:30 GMT. T MATSUMOTO is a senior OAA Mars observer since the 1950s, and known as one of SAHEKIs disciples. On 15 August he used a 28cm SCT to take a Video series of images of Mars by a TRV900 beyond 15h GMT. He then changed to watch the surface by the naked eyes by the use of the binocular-type eyepieces at 600 and readily found around at 15:30 GMT, as he moved his keen eyes from Hellas to Syrtis Mj, there was shining a white spot near the Huygens crater. Its diameter was about 0.5 arcsecs, and twinkled (due to seeing condition). The white tint of the spot reminded him of a bright colour of a button made of shell. It was slightly brighter than the spc. Unfortunately the planet was concealed by a gathering cloud after 4 or 5 minute watching. At around 16h GMT, the planet reappeared, but the seeing turned to be poorer, and so he changed his scope to a 54018cm refractor, but no trace of the flare was found again. He suspected it at most lasted for about 20 minutes. During his watching, the spot did not move in reference to other markings, and it really twinkled so that he did not think it was a ghost. He furthermore supposes it was not like a radiation, but just a reflection. Here we show a sketch made based on his memory after the event. The Video camera and his binocular-type ocular can be removed and attached within 30 seconds, and so we here also show an image made by the TRV 900 just before his discovery. We are not sure that this area has been listed as any area which shows flares like Edom or other well-known spots. We so propose we should henceforward to list and watch around this spot as a candidate of possible flashing area.



T Naha: As reported above, IWASAKI (Iw) visited Naha at the beginning of August to join the checking team of the possible flares near the Solis L region. At the same time he enjoyed the good seeing of the planet especially on 2 August by the use of a well collimated 35cm SCT. The angular diameter was then 22.6 arcsecs, and we suppose he was able to catch the best view of the Martian surface ever since he began to observe the Martian surfaces (from 1984). On the evening the dust at Capri Cornu was passing the CM, and the delicate shadowy part of the spc was coming. After the Typhoon No 10, TSUNEMACHI (Ts) visited Naha to watch the planet on 11 August. The angular diameter was increasing rapidly and was already 24 arcsecs, and the surface was showing much details night by night. It was a great surprise to her that the Zwei nails of Aryn were always apparent. Here we cite one of her drawings (among a total of 34 drawings obtained during a few days). Ts also detailed such minor spikes as Orestes and Electra (named by S EBISAWA) and/or Iuvent Fons which were all easily caught this time. It was possible for her to chase up to Aurea Cherso. In this way the planet Mars in August 2003 was very rare, special and great.



he next issue shall treat the observations made in the second half of August 2003 from 16 August (λ=242Ls, δ=24.5") to 31 August 2003 (λ=252Ls).. During the period the planet makes an unprecedented closest approach on 27 August with δ=25.1".

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