th Report:
The CMO/OAA Observations made during a fortnight period from
1 August 2003 (232°Ls) to 15 August 2003 (242°Ls)
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=232°Ls to 242°Ls 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 20°S/19°S, 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 13.5°Sà14.5°S.
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.
Contents
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
Hellas
Trinacria
M Cimmerium
The Ætheria
Dark Patch
Arsia White
Cloud and Olympus Mons
Others
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/32×32cm 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/28,32×25cm 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, 1045×41cm F/6.9
spec
BIVER, Nicolas (NBv) Versailles, France
2 Colour Drawings (9, 12 August 2003)
510×26cm 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, 680×43cm F/7.8 speculum
CAPARRÓS, Angel (ACp) Málaga, España
3 CCD Image
(9, 10, 15 August 2003)
25cm spec with a ToUcam
CARLOS CASADO, Juan (JCs) Figueres, España
4 CCD Images (5, 6, 7, 10 August 2003)
f36×15cm 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,
24×18cm 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, Isêre, France
4 CCD Images (4, 12/13 August
2003)
f/27×50cm spec with a KAF400 chip camera
FRASSATI, Mario (MFr) Crescentino (VC), Italia
4 Drawings (1, 5, 9, 15 August 2003) 250, 400×20cm SCT
FUMEGA UCHA, Camilo (CFm) Ourense, España
4 CCD Images (1, 7, 10, 12 August 2003)
f/25×31cm spec with a ToUcam
GRAFTON, Edward A (EGf)
Houston, TX, USA
3 Sets of CCD Images (1, 2, 11 August 2003)
f/27, 39×35cm SCT with an ST-5C
GRAHAM, David L (DGh) North Yorkshire, UK
1 Colour Drawing+1 Note* (2*, 3 August 2003)
160×15cm 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,
280×25cm spec/ 20cm SCT
HILL, Harold (HHl) Lancashire, UK
2 Colour Drawings (9, 14 August 2003)
270,
290×14cm 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 àFukuoka, Japan
22 Drawings (1+, 2++, 12
August 2003) 400×21cm speculum
+400, 530×31cm spec, 415×21cm spec chez ISHADOH,
++430×35cmSCT chez TABATA; 530×25cm F/8.5spec chez Mn
KARRER, Michael (MKr) St Radegund, Österreich
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, 47×20cm 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/84×20cm Dall-Kirkham
with a ToUcam
LAU, Canon (CLa)
Hong-Kong
1 CCD Image (9 August 2003) f/59×35cm SCT with a ToUcam
LAU, Patrick (PLa) Hong-Kong
2 Drawings (9, 10 August 2003) 300, 340×25cm 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/25×30cm spec with a Philips ToUcam
MATSUMOTO, Tatsujiro (TMt) Amagasaki, Hyogo,
Japan
1 Drawing and 2 CCD Images (15 August 2003)
600×28cm SCT & 540×18cm 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, 550×25cm F/8.5 speculum, * 280×25cm SCT
+400, 530×31cm spec, 415×21cm spec chez ISHADOH,
++430×35cmSCT chez TABATA
MOORE, David M (DMr) Phœnix, AZ, USA
4 Sets of CCD Images (3, 5, 9 August 2003)
f/50×25cm speculum with a ToUcam Pro
MORITA, Yukio (Mo) Hatsuka-ichi, Hiroshima, Japan
4 Sets of CCD Images (1, 2, 12 August 2003)
f/50×25cm speculum equipped with an ST-5C
MURAKAMI, Masami (Mk)
Yokohama,
Kanagawa, Japan
19 Drawings (2*, 3*,
6 August 2003)
*350×15 cm spec, 400×20cm spec
NAKAJIMA, Takashi (Nj) Fukui,
Fukui, Japan
8 Drawings (2, 10 August 2003) 400×20cm ED Goto refractor*
*Fukui City
Observatory, Fukui
NARITA, Hiroshi (Nr) Kawasaki, Kanagawa, Japan
9 Drawings (2, 3, 4, 6, 7, 10 August 2003) 400×20cm refractor
NIKOLAI, André (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/34×15cm Maksutov with
a ToUcam
PARKER, Donald C (DPk) Miami, FL,
USA
6 Sets of CCD Images (12, 13 August 2003)
f/55×41cm 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/32×20cm 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/48×13cm Starfire refractor with a ToUcam
RODRÍGUEZ RAMÍREZ, Francisco A (FRd) Gran
Canaria, Canary Islands,
España
1 CCD Image (15 August 2003) 20cm SCT with a ToUcam
SÁNCHEZ, Jesús R (JSc)
Córdova, España
11 CCD Images (1, 4, 9, 10, 15 August 2003)
f/40,45×28cm SCT with a ToUcam
SCHMUDE, Richard W,
Jr (RSc) GA, USA
3 Drawings (4, 14, 15 August 2003) 230×10cm refractor
SCHULZ, Robert (RSz) Wien, Österreich
1 CCD Image (3 August 2003) 31cm spec with a ToUcam
SEIP, Stefan (SSp) Stuttgart, Deutchland
2 CCD Images (2 August 2003)
f/32×25cm Mak-Cass/f/43×16cm 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)
270×20cm F/10 SCT
STÖGER, Jürgen (JSt) Katzelsdorf, Österreich
1 CCD Image (10 August 2003) f/40×10cm Refraktor with a ToUcam
SURO, José (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, Gérard (GTc)
Hattstatt,
France
6 Drawings (2, 3, 5, 7, 9, 13 August 2003) 330×28cm SCT
TSUNEMACHI, Hitomi (Ts) Naha, Okinawa,
Japan
34 Drawings (11, 12, 13, 15 August 2003)
530, 550×25cm F/8.5 speculum
VALIMBERTI, Maurice P (MVl) Melbourne, Australia
8 CCD Images (1, 2, 5, 9, 15 August 2003)
f/34×35cm SCT with a Philips ToUcam Pro
Van Der VELDEN, Erwin
(EVl) Brisbane, Australia
4 CCD Images (10, 12, 13 August 2003)
f/31×20cm SCT with a Vesta
Pro modified
WALLER, Skip (SWl)
Dallas, TX, USA
2 CCD Images (8, 10 August 2003)
f/50×25cm SCT (LX200) with
a ToUcam Pro
WARELL, Johan (JWr) Tucson, AZ,
USA
3 Drawings (5, 6, 10 August 2003)
260×25cm SCT (LX200)
1 CCD Image (10 August 2003) f/23×25cm SCT with a ToUcam
WIENECKE, Marcus (MWn) Fröndenberg, Deutchland
2 CCD Image
(9, 15 August 2003)
f/20×25cm SCT (LX200)
with a ToUcam Pro
WILLIAMSON, Thomas E (TWs) Alburquerque,
NM, USA
3 Sets of CCD Images (1, 10 August 2003)
f/45×20cm 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=094°W) to 18:27
(ω=111°W) 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 Rei’ichi KONNAI (né 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=225°Ls (he obtained also excellent results about the Solis L dust storm
in 1973): KONNAI recollected and assured that this year’s 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=260°Ls,
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=205°Ls, 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=268°Ls. The atmospheric pressure increased rather
linearly from λ=180°Ls to λ=270°Ls: 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=180°Ls to λ=270°Ls. 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=145°W on 7 August (λ=237°Ls) 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=137°W.
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=231°Ls) at Achillis Pons looked to cause another rise of dust at Chryse
on 30 July (λ=231°Ls) whose early morning state was well observed in the US. On 31 July
(λ=232°Ls) 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=069°W 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=232°Ls), 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=342°W, BATES (DBt) at ω=345°W, WILLIAMSON (TWs) at ω=351°W, SHERROD (CSr) at ω=353°W, and of TWs at ω=002°W. TWs’s 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=060°W. Successively, MORITA (Mo) took at ω=073°W, and PACE (BPc) at ω=081°W. ASADA (As)’s image at ω=104°W 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=057°W, while the planet was still low. Iw first checked the dust at Eos from
ω=062°W, and then watched at ω=072°W, 082°W, …
(and thus every 40 minutes ten times until ω=149°W 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=101°W.
On 2 Aug
(λ=233°Ls),
the dust was rather conspicuous at Capri Cornu. EGf’s image at ω=328°W 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=034°W. And then an excellent series of
images was produced by AKUTSU (Ak) at
ω=037°W, 047°W, 056°W, 066°W, 076°W, 088°W, 097°W, and
106°W (eight images!). The dust from Eos to Capri Cornu is
clearly shown there. The images are stable from ω=056°W, or 066°W, and
also show an extension of dust over Pyrrhae R. BUDA (SBd)’s image at ω=042°W is also suggestive. KUMAMORI (Km) took at ω=049°W and 061°W, and ASADA (As) also took successively at ω=051°W, 062°W, 070°W, 080°W, 089°W, 099°W, 110°W:
The images are stable around from ω=070°W. MORITA (Mo) took at ω=065°W. At Okinawa,
we were to kill two birds with one stone: We were gathering at Tabata’s 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=038°W. 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=043°W(Iw), 048°W(Mn), 053°W(Iw), 058°W(Mn), 063°W(Iw), 068°W(Mn), 073°W(Iw), 077°W(Mn), 082°W(Iw), 087°W(Mn), 092°W(Iw). Then we moved to MINAMI’s observing site and observed until ω=136°W(Mn), 140°W(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=090°W. We should say however the brightness did not
suggest any of the big dust.
3 Aug (λ=234°Ls), no other observation of dust was
made than in Asia. Ak took a series of images at ω=028°W, 036°W, 046°W, 056°W, 071°W, and 080°W.
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=029°W, 039°W, 049°W, 059°W, 068°W, 078°W, 098°W, 117°W, 127°W (rain
showers twice), and Km took at ω=054°W, 072°W, 086°W. ASADA (As) also shot at ω=065°W, 075°W, 086°W. 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=235°Ls),
Mn observed at ω=040°W, 050°W,
059°W, 069°W, 079°W, 089°W, 098°W, 108°W: 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=044°W, 080°W, 099°W
well show a bright
core inside the dust at Capri Cornu which was apparent even near the
terminator. On 5 Aug (λ=235°Ls), Typhoon No 10 was approaching
and Mn checked the area no more than
three times at ω=031°W, 041°W, 050°W. The horn area was seen but the dust
was quite dull. On the day, MVl took
the ccd images at ω=009°W, 025°W, SBd at ω=016°W, Km at ω=035°W, 044°W, and As at ω=036°W, 047°W, 058°W: None showed the
preceding-day’s brighter core inside Capri Cornu. On the same day, MOORE (DMr) secured images at ω=319°W as well as Tim PARKER (TPk)’s at ω=343°W, 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=236°Ls) at ω=074°W, 081°W. There seems to show a local
expansion at the bulge of the bugle. On 7 Aug
(λ=236°Ls),
Ak produced a series at ω=001°W, 011°W, 021°W, 039°W, 049°W. 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=026°W, and OKANO (Ok) at ω=032°W 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=238°Ls), 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=004°W～029°W, and otherwise those by MVl at ω=004°W, BPc at ω=025°W, and Canon LAU (CLa) at ω=049°W. From Okinawa, we watched from the
angles of ω=355°W, 005°W, 005°W, 024°W, 034°W, 044°W, 053°W, and 063°W.
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=027°W on 13 Aug (λ=240°Ls) 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: EGf’s excellent image on 2 Aug (λ=233°Ls) at ω=328°W well indicated that Novus Mons had
already separated from the spc. See also the magnified figure. BATES’s (DBt)’s
image on 3 Aug (λ=234°Ls) at ω=324°W also suggests the detachment. See
also the images of the spc on MOORE (DMr)’s
on 3 Aug (λ=234°Ls) at ω=329°W(R), as well as on TPk’s on 5 Aug at
ω=342°W. The season λ=233°Ls 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=242°Ls. The present
writer’s Observing Note after the Typhoon made on 9 Aug (λ=238°Ls) at
ω=355°W 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=249°Ls by E C SLIPHER. Later observations, including those by
LOWELL and BARNARD in 1894, seem to indicate λ=251°Ls as a mean value.
However, according to ANTONIADI’s list, the season by LOWELL and BARNARD in
1894 was around λ=220°Ls. The result of ANTONIADI in 1909 implied
λ=247°Ls, while LYOT’s one in 1924 pinned down
λ=242°Ls. 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=255°Ls, 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=237°Ls),
WALLER (SWl)’s
at ω=282°W,
DBt’s at ω=297°W as well as CHAVEZ (RCv)’s image on
10 Aug at ω=249°W and DBt’s image on 11 Aug (λ=239°Ls) at ω=231°W. The angle of the image of WARELL (JWr) on 10 Aug (λ=238°Ls) at ω=277°W is good, but the image looks
slightly embossed. According to our observations on 15 Aug (λ=242°Ls) at
around ω=287°W, the follower (rotationally preceding) was still remaining,
while near the terminator it became very dimmed as recorded on 12 Aug (λ=248°Ls)
at ω=328°W and so on. The aspects at λ=240°Ls~242°Ls
this year were caught by Km, Mo, and EVl on 12 August at ω=346°W, ω=353°W, and ω=358°W respectively, and MVl and SBd on 15 Aug (λ=242°Ls) at ω=287°W/310°W, and at ω=297°W 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=239°Ls) at
ω=337°W 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=030°W 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=235°Ls) at ω=040°W. See Argenteus Mons on the images on 7 Aug
(λ=236°Ls) at ω=026°W by BPc and at ω=032°W by OKANO (Ok) as well as on MVl’s
image on 9 Aug (λ=239°Ls) at ω=004°W, Canon LAU (CLa)’s image at ω=049°W, Patrick LAU (PLa)’s drawing at ω=025°W. Further westward, there is a
bright spot near Ω=080°W to the south of Solis L. See Km’s images on 3 Aug (λ=234°Ls) at ω=072°W, as well as on 4 Aug
(λ=235°Ls) at ω=080°W. Furthermore at around
Ω=150°W, we meet Thyles Mons. Its shape was depicted on the images by
PELLIER (CPl) on 6 Aug
(λ=236°Ls) at ω=172°W, on 9 Aug (λ=237°Ls) at ω=140°W, as well as on LAZZAROTTI (PLz)’s 10 Aug (λ=238°Ls) at ω=140°W. DPk’s images on 13 Aug (λ=240°Ls) at ω=190°W also gives us a clear cut image.
See also KARRER (MKr)’s
on 10 Aug (λ=238°Ls) at ω=147°W. The peripheral bright spot shown
on the drawing by FRASSATI (MFr) on
15 Aug (λ=242°Ls) at ω=129°W as well as on the image by TATUM (RTm) on ω=170°W is Thyles Mons. If seen further
west of ω=200°W, the contour is made of several light beads including
Thyles Collis. For instance, CPl’s
images on 1 Aug (λ=232°Ls) at ω=230°W and SEIP
(SSp)’s on 2 Aug
(λ=233°Ls) at ω=233°W 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=230°W. These can be seen
if compared with the periphery of the spc on the images of EGf on 11 Aug (λ=239°Ls) at ω=231°W as well as on DPk’s on 12 Aug (λ=240°Ls) at ω=231°W. Here we cite one from CPl’s at λ=232°Ls and EGf’s at
λ=239°Ls. Also the images by HANON (DHn) on 9 Aug (λ=237°Ls) at ω=237°W as well as DBt’s on 11 Aug (λ=239°Ls) at ω=238°W 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=230°Ls, and so the
observation was pressing from 1 August (λ=232°Ls). The present writer (Mn) as well as Iw watched up to the angle
ω=135°W, and noticed that the western side of Thyles Mons had become less
bright. On 2 Aug (λ=233°Ls) Mn
observed with Iw
up to ω=136°W and obtained similar result though the thawing was
inadequate. On 4 Aug (λ=235°Ls), we saw the morning side of the spc looked
slightly shadowy (partly because of the airborne dust) from ω=050°W. Since
we thought the season λ=235°Ls 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 158.3°W), 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." ESg’s Observing Note on 7 Aug (λ=236°Ls) at
ω=158°W records that the boundary looked sharp. She also made a similar
observation one day after at ω=145°W (23:50GMT on 7 Aug). KOWOLLIK (SKw) was observing also on 6/7 Aug
(λ=236°Ls), and her series of ccd images showed
that the right-hand side of the spc had been less bright at ω=147°W, 156°W, and 166°W. This aspect is
evident and definite also on the images by CPl
on 9 Aug (λ=237°Ls) at ω=140°W(R), 142°W(G), by PLz and his comrades on 10 Aug
(λ=238°Ls) at ω=140°W, by MKr at ω=147°W, and by PBl at ω=154°W (Thyles Mons is made of two bright
spots on CPl’s images). PLz’s IR image on
the day at ω=114°W suggests well how the aspect will appear later from
ω=140°W.
As stated previously, as the season proceeds to
λ=240°Ls, the east of Ω=230°W becomes shadowy and so we can easily
catch the area where the thawing is rapid. DPk’s
images on 13 Aug (λ=240°Ls) at ω=190°W~204°W show the area from Thyles
Mons to this point and hence these images will be compared later with the later
thawed-away case. RCv’s
image on 15 Aug (λ=242°Ls) at ω=187°W, since this being harder processed
than DPk’s, suggests well the area to
be thawed away.
If we see the spc from ω=230°W to 320°W, 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=234°Ls) ω=281°W, and this gives the case in good
contrast. DMr’s
images on 5 Aug (λ=235°Ls) at ω=318°W also show this. It is also clear on
images on 8 Aug (λ=238°Ls) by SWl at ω=282°W, and by DBt at ω=297°W. The angle is slightly shallow, but
DHn’s image
on 9 Aug (λ=237°Ls) at ω=237°W also shows the contrast. The images
on 11 Aug (λ=239°Ls) by EGf at ω=231°W as well as by DBt at ω=238°W prove clearly the shadowy area from
the far different angles. Finally, on 15 Aug (λ=241°Ls), MVl’s images at ω=287°W～311°W, and SBd’s at ω=297°W show the
good images of the spc. Note that the thawed-away area shows a tint of ochre. This may be check on EVl’s image on 13 Aug (λ=240°Ls) at
ω=315°W, 331°W, 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=123°W～129°W. On 1 Aug (λ=233°Ls), Mn caught the area at ω=116°W, 126°W, 135°W (also on 2 Aug at
ω=126°W 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. Km’s image
on 3 Aug (λ=234°Ls) at ω=123°W shows the deformed area of the
tadpole, and CPl’s images on 13 Aug
(λ=240°Ls) at ω=123°W may show the final stage. MKr’s image on 12
Aug at ω=117°W 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=235°Ls) at ω=050°W, the outskirts of Argenteus Mons showed a weak
cascade, and on 13 Aug (λ=240°Ls) at ω=358°W, another cascade was
seen to the south of Noachis. On 12 Aug (λ=248°Ls) at the ω=328°W
session, we saw a projection toward north from the outer side of Novus Mons. On
14 Aug (λ=241°Ls) at ω=301°W, we observed a projection from the top
tip of Novus Mons. Maybe the projection-like tip of Novus Mons seen on MVl’s images on 15 Aug (λ=241°Ls)
at ω=277°W, 310°W as well as on SBd’s image at ω=297°W 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=235°Ls) at around ω=040°W, 050°W,
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=242°Ls) at ω=287°W~ and this was also
confirmed by TSUNEMACHI (Ts) by the
same telescope. Even at ω=000°W (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=223°Ls) at ω=234°W~279°W, 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=223°Ls) at ω=229°W~273°W 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=232°Ls) at ω=206°W~270°W, 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=238°Ls) at ω=256°W. EGf’s LRGB images on 11 Aug (λ=239°Ls) at ω=231°W 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=238°Ls) at ω=327°W, 336°W, 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=346°W (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, CPl’s
images taken on 1 Aug (λ=232°Ls) at ω=228°W~267°W 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 SWl’s
on 8 Aug
(λ=237°Ls) at ω=282°W, DMr’s on 9 Aug (λ=238°Ls) at
ω=275°W, 284°W, RCv’s and SWl’s on 10 Aug (λ=238°Ls)
respectively at ω=249°W, and at ω=263°W, and DBt’s on 11 Aug (λ=239°Ls) at ω=238°W are all show these aspects. Among
them, the images by EGf made on 11
Aug (λ=239°Ls) at ω=231°W 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 MOC’s
images), and the complex description of the eastern part of M Hadriacum is
excellent. DPk’s images on 12 Aug
(λ=240°Ls) at ω=234°W 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=232°Ls) at ω=245°W.
Her friend
NIKOLAI (ANk)
also showed it on 2 Aug at ω=219°W, 234°W. BALDONI (PBl), using a
18cm Mak-Newton showed it on 3 Aug at ω=200°W. PELLIER, with a
18cm Newton,
not first but also spiked down on 4 Aug (λ=234°Ls) at ω=197°W, and on 6 Aug (λ=236°Ls) at ω=192°W in full length. By the use of a
15cm CASADO (JCs)
showed it on 5 Aug at ω=191°W. 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 EGf’s ccd images on 11
Aug (λ=239°Ls) at ω=232°W (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 MIYAZAKI’s
drawing in 1988).
The Aetheria
Dark Patch: Already it was several times noted that
the Ætheria 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 EGf’s image on 11 Aug
(λ=239°Ls) at ω=231°W and DPk’s on 12 Aug (λ=239°Ls) at ω=234°W and so on.
Arsia
White Cloud and Olympus Mons:
This period, few observations were made about the evening Tharsis. CPl’s images on 9 Aug (λ=237°Ls) at
ω=140°W, 170°W 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=241°Ls). A critical case was obtained by DPk on 13 Aug (λ=240°Ls) at ω=190°W, 193°W: 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. CSr’s
image on 15 Aug (λ=241°Ls) at ω=187°W 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 Fœlix
mpressives:
One of most impressive files this period is AKUTSU’s images which were taken on
2 Aug (λ=233°Ls) at ω=037°W~106°W:
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). KUMAMORI’s Solis L on 6 Aug (λ=236°Ls) at ω=074°W is also
impressive: Note this was taken by the use of a homemade 20cm Dall-Kirkham when δ＝23.3".
Abroad, PELLIER
(CPl)’s files are all attractive:
especially the file made on 1 Aug (λ=232°Ls) at ω=206°W~270°W is
the most
impressive.
VALIMBERTI (MVl)’s image on 9 August (λ=237°Ls) at ω=004°W was
fascinating and at last on 15 Aug (λ=241°Ls) he gave a final impression
with the images at ω=277°W, 310°W.
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=20.1°S 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 35°N)
|
(GMT)
|
13:00
|
14:00
|
15:00
|
16:00
|
17:00
|
18:00
|
19:00
|
20:00
|
21:00
|
|
29 July
|
067°W
|
082°W
|
096°W
|
111°W
|
126°W
|
141°W
|
155°W
|
170°W
|
185°W
|
|
30
|
058°W
|
073°W
|
087°W
|
102°W
|
117°W
|
131°W
|
146°W
|
161°W
|
176°W
|
|
31
|
049°W
|
064°W
|
078°W
|
093°W
|
108°W
|
122°W
|
137°W
|
152°W
|
167°W
|
|
01 Aug
|
040°W
|
055°W
|
069°W
|
084°W
|
099°W
|
113°W
|
128°W
|
143°W
|
158°W
|
|
02
|
031°W
|
046°W
|
060°W
|
075°W
|
090°W
|
104°W
|
119°W
|
134°W
|
149°W
|
|
03
|
022°W
|
037°W
|
051°W
|
066°W
|
081°W
|
095°W
|
110°W
|
125°W
|
140°W
|
|
04
|
013°W
|
028°W
|
042°W
|
057°W
|
072°W
|
086°W
|
101°W
|
116°W
|
131°W
|
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 (Mk’s 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 Ishadoh’s 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 Tabata’s 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 Ishadoh’s.
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 Id’s 31 reflector). On 2 August, we
gathered at Tabata’s 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 Tabata’s by 17h GMT, and then
Iw and Mn moved to Minami’s watching roof site (quite near Tabata’s) 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 Wakugawa’s 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=059°W to
19:35 GMT ω=127°W;
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=043°W~18:00 GMT ω=095°W, 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=042°W to
19:00 GMT ω=110°W). Here we cite a ToUcam image at 15:27GMT with
ω=058°W. 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 Kobé, 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 SAHEKI’s 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 540×18cm 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 Iuventæ 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=242°Ls, δ=24.5") to 31 August 2003 (λ=252°Ls).. During the period the planet makes an unprecedented
closest approach on 27 August with δ=25.1".
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