2001 Mars Observation Reports -- #10--
OAA MARS SECTION
Mars Observations
in the First Half of June 2001
from 1 June 2001 (171°Ls) to 15 June 2001 (179°Ls)
based on the article published in CMO #246 (25 June 2001)
by Masatsugu MINAMI, Director of the OAA Mars Section
T |
HE angular diameter
increased from 19.3 arcsecs to 20.6 arcsecs during the period. The moment the
We acknowledge receipt of the observations this period
as follows:
AKUTSU, Tomio (Ak) Karasuyama,
4 Sets of CCD Images (2, 4,
ASADA, Tadashi
(As) Munakata,
4 Sets of CCD Images (8, 11 June
2001) 30cm spec equipped with a Lynxx
PC
BARNETT,
John H (JBn) VA,
3 Drawings (2, 8 May; 11 June
2001) 270, 360x 18cm refractor $
BATES, Donald
R (DBt)
3 Colour Images (3, 11,
BIVER,
Nicolas (NBv)
13 Colour Drawings (18, 19, 25, 28,
30 May; 1, 5, 10, 11, 12, 13 June 2001)
310x 20cm spec, 330x 26cm speculum
CAVE,
Thomas R (TCv)
2 Drawings (31 May;
CIDADÃO,
António José (ACd)
2 Set of CCD Images (9 June
2001) 25cm LX200SCT equipped with an
ST-5C + AO
Di
SCIULLO, Maurizio (MSc)
1 Set of CCD Images (
FALSARELLA, Nélson (NFl)
4 Drawings (4, 5, 8 June 2001) 325x 20cm speculum
2 CCD Images (8, 11 June 2001) 20cm speculum + AVA ASTROVID 400
GRAFTON,
Edward A (EGf)
2 Sets of CCD Images (3,
HERNANDEZ,
Carlos E (CHr)
3 Sets of Drawings (
HIGA, Yasunobu (Hg)
21 Video Images (2, 10, 12, 15 June
2001) 25cm f/6.7 spec with Sony VX-1000
HIKI,
Toshiaki (Hk) Minowa,
3 Drawings (
ISHADOH,
Hiroshi (Id)
18 Drawings (1, 2, 4, 10, 12, 13, 15
June 2001) 340, 400, 530x 31cm speculum
ISHIBASHI,
Tsutomu (Is)
5 Sets of Colour Photos (15 April; 12, 20,29
May;
31cm
f/6.4 speculum Fujichrome Provia 400
KUMAMORI,
Teruaki (Km)
10 CCD Colour Images (2, 8, 11, 12
June 2001) 20cm Dall Kirkham with a Sony PC-5
MELILLO,
Frank J (FMl)
3 Sets of CCD Images (1, 4,
MINAMI,
Masatsugu (Mn)
43 Drawings (1, 2, 3, 9, 11,
MORITA,
Yukio (Mo) Hatsuka-ichi,
37 Sets of CCD Images (1, 2, 3, 6,
7, 9, 11, 12, 15 June 2001)
f/50 25cm speculum equipped with
an ST-5C
MURAKAMI,
Masami (Mk)
6 Drawings (2, 3 June 2001) 320x 20cm speculum
NAKAJIMA,
Takashi (Nj)
17 Drawings (2, 3, 9
NARITA,
Hiroshi (Nr)
4 Drawings (2, 3,
PARKER, Donald
C (DPk)
3 Emails (7, 8, 9 June) on the
5 Sets of CCD Images (11, 14 June
2001)
f/44 41cm Meade SCT equipped with a Lynxx PC
TEICHERT,
Gérard (GTc)
2 Drawings (5,
TSUNEMACHI,
Hitomi (Ts) Yokohama, Kanagawa,
Japan
8 Drawings (2 June 2001) 360x 12.5cm Fluorite refractor
*
$
A :
The
biggest and most important topic in this period was the successful detection of
the Edom brightening by Don PARKER and others at the Florida Keys. Tom DOBBINS
and W SHEEHAN pointed out in the May issue of the S&T (in
their article "The Martian-Flares Mystery") that some of the sharp
flares hitherto known were possibly due to rare cases of the Sun-glints, and
suggested one of rare cases could possibly happen this June at Edom facing to
the US. To confirm the hypothesis, they planed an expedition to a good milieu
in
According to DPk
(#245 p3016) and TDb in this issue, after two nights passed in
vain, they finally encountered with a series of wonderful pulsations at Edom on
7 June from 6:40 GMT ( ω=330°W) to 7:20 GMT ( ω=342°W): The flares
showed about 3 second durations and repeated at 10 to 15 second intervals. They
used a 30 cm Meade STC equipped with a Video Camera as well as two 15cm
Newtonians for visual observations. The pulsations were witnessed at the
eyepieces as well as on the monitor. This success was beyond all praise, and
not only justified the forgoing Japanese 'relegated to the fringe'
observations, but added an important discovery of 'pulsations'.
Don PARKER hurried to his PC, and sent out the news at 7:54 GMT to
The story did not end, and the success was incomparable since the flares
were also observed on the following 8 June: They report there occurred two
peaks; the first was from 7:00 GMT (at ω=326°W) to 7:20 GMT (
ω=331°W), and then the second peak came at 7:53 GMT ( ω=340°W) and
ended at 8:24 GMT ( ω=347°W). See further details DPk's description in #245 p3016 and TDb's ones at p2020 and in this issue. They tried the
observation on 9 June, but the flares was no longer seen.
On 7 June at 7h GMT, φ read 1.78°N while Ds was
2.53°N, and hence, if the 'mirror' was laid horizontally (highly possible
because of democratic gravitation), the position of the mirror was at 2.16°N.
On 8 June at 7h GMT, φ and Ds read 1.98°N, 2.29°N respectively, and hence the position
is suggested at 2.13°N. On the other hand, there was no detection on 5, 6 June
around at 7h GMT and on 9 June at 7h GMT, and so we may say that the latitude
of the position of the mirror was between 2.13°N and 2.16°N, or was not located
outside the zone from 2.11°N to 2.18°N. The value of 2°N was really reminiscent
of the position of Edom in older maps, but the recently established USSG map
puts the Schiaparelli crater or Edom Pr on the southern hemisphere. So we may
suppose the mirror was not horizontal or the flared position was not
necessarily inside Edom Pr. It is often suggested that the case detected by
Tsuneo SAHEKI on 1 July 1954 at 13:15 GMT was similar, but we should remember
there are some differences: As noted in CMO #242 p2973, the case in 1954, φ=2.11°N while Ds was on the other sphere at Ds=3.40°S,
and so the virtual position was at 0.65°S if horizontal. And in the 1954 case,
we can suppose the flare occurred only that once (SAHEKI complained at that
time to hear that I TASAKA was observing at the same time with SAHEKI, but did
not see the flare. It was however almost impossible, if the spontaneous flare
occurred only once, because any visual observer often turns his eye away from
the eyepiece down to his drawing book during one session). However the SAHEKI
case was unique in that the flash was durable only within a few seconds, while
other cases recorded a few minute duration, and so the mechanism must share
with the present case. Inquired of the present writer, he is of an opinion
(submitted to TDb) that the matters naturally laid down are more
easily found from the above, and we can more easily find a mirror or mirrors
(if many they more probably face upward) to glare if we locate our position
right just above the place where the mirrors are concealed having our back to
the Sun. Nature is often not simple, and the mirror may be inside a deep well
or mirrors are laid along inside a deep trench. Then probability implies the
case Ds=De as the most probable case, and the durations from
the same point may imply a presence of convex mirrors. SAHEKI's case is
therefore heterodox, and may be quite difficult to predict (if in such a case
where a part of the wall of the trench is broken) compared with the simpler
case of Sanenobu FUKUI in 1958 (as so done in DOBBINS and SHEEHAN). The present
case was the analogue of
B :
The critical season 176°Ls came on 10, 11 June: On 10 June, HIGA (Hg) felt that the south polar region (spr) was free from the hood. The evening side of the spr looked definitely free from the hood. The volatilized
trace of Argyre was also observed outside the cap.
MORITA
(Mo) secured good images (including the detailed LRGB
images) on 11June (176°Ls) and 12 June (177°Ls) at ω=081°W and ω=042°W respectively,
where, the spc appears with some details. Mo took an image of a trace of Argyre on 5 June (178°Ls) at
ω=022°W.
Don PARKER (DPk), after his return from the historical stays at the
Florida Keys, produced interesting and (may-become-important-later) images on 11 June
(176°Ls) at ω=271°W, 289°W, 295°W, and 305°W. They all show strange
DPk's images on 14 June
(178°Ls) show that the western corner of
Around 2 June (171°Ls), HIKI, ISHADOH, ISHIBASHI, KUMAMORI,
C :
BARNETT (JBn) is a member of the Richmond Astronomical Society
and is a friend of
CIDADÃO (ACd)'s images are made on 9 June at ω=236°W, 242°W
where Ausonia looks bright.
BATES (DBt)
is one of the last persons who use emulsions (similarly to ISHIBASI (Is) in
T |
he next issue shall
review the observations during a fortnight period from 16 June (179°Ls) to 30
June 2001 (187°Ls). Our CMO Web-Site has a Gallery Page where some new Mars images are flashed before
our reviewing. We hope every CCD image is emailed in a jpg file with a file
name beginning with the observer's name to vzv03210@nifty.com
as well as to cmo@mars.dti.ne.jp.
Drawings are preferred to be sent in an A4 sized format with just one drawing
on one sheet.
Reports will be acknowledged if air-mailed to
M MINAMI at Mikuni
(ask the mail-address through vzv03210@nifty.com
) .
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