2001 Mars Observation Reports -- #20--


CMO Mars Observations

in the Second Half of January 2002 and the First Half of February 2002
from 16 January 2002 (310Ls) to 15 February 2002 (327Ls)
based on the article published in CMO #257 (25 February 2002


Masatsugu MINAMI, Director of the OAA Mars Section


ERE we deal with the period from

16 January 2002 (310Ls) to 15 February 2002 (327Ls)

in which the apparent angular diameter went down from 5.9" to 5.1". It was not so hopeless still because the apparent declination was increasing (it went up across the celestial equator from -1.3 to 7.8 during the period). The problem was rather the winter weather. The central latitude was down from 26.5S to 24S. The phase angle was also down from 37 to 32.


HE activity of Don PARKER (DPk) is still remarkable. The Japanese observations turned less active, but KUMAMORI (Km)'s images proved good. We hear the weather was unstable even in the districts facing to the Pacific Ocean, not to mention at the rear side district.

ISHADOH, Hiroshi (Id) Naha, Okinawa, Japan

6 Drawings (30, 31 January; 3, 4, 6, 13 February 2002)

400, 530x 31cm speculum


KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan

9 CCD Colour Images (19, 24 January; 1, 6, 15 February 2002)

60cm Cassegrain# with a Sony TRV-900


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

1 CCD Images (26 January 2002)

20cm SCT with a Starlight Xpress MX5

MINAMI, Masatsugu (Mn) Fukui, Japan

26 Drawings (19 January; 4, 6, 13, 15 February 2002)

600, 480, 400x 20cm ED Goto refractor *


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

2 Sets of CCD Images (26 January; 12 February 2002)

f/40 36cm F/13.5 Cassegrain with a Starlight Xpress HX5

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

8 Sets of CCD Images (22 January; 1, 3, 9, 12, 15 February 2002)

f/50 25cm speculum equipped with an ST-5C

MURAKAMI, Masami (Mk) Fujisawa, Kanagawa, Japan

3 Drawings (9, 10 February 2002)

300x 10cm ED Nikon refractor

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

10 Sets of CCD Images (18, 21, 25, 28 January; 2, 3 February 2002)

f/44 41cm F/6 Newtonian equipped with a Lynxx PC

PEACH, Damian A (DPc) Chatham, Kent, UK

1 Set of CCD Images (15 February 2002)

f/29 31cm Meade SCT with an ST-5C


TSUNEMACHI, Hitomi (Ts) Yokohama, Kanagawa, Japan

4 Drawings (23 January 2002)

360x 12.5cm Takahashi fluorite refractor


# Sakai City Observatory

* Fukui City Observatory

Observations from the US:

 Don PARKER (DPk) at Florida made observations on 18 January (312Ls) at ω=228W, 231W, and 234W where M Cimmerium is wholly shot. Hesperia and M Tyrrhenum look classical. Eridania shows its surface colour. M Chronium and M Hadriacum are dark evident. The dark marking at theria is rather large (it was before shot on DPk's images on 11 December at ω=237W - #254 p3190). Is it similar to the scale in 1975?
  On 21 January (313Ls),
DPk observed at ω=201W & 208W where Scamander separates Electris and Eridania. The spc is dull, and unseen in B. The spc is not distinct also on the DPk images on 25 January (316Ls) at ω=165W where M Sirenum and M Cimmerium are shown connected.

  On 28 January (318Ls) DPk made his B day's shot at ω=135W & 139W: The former is associated with a grid system, and this proves the latitude of Solis L is located between 20S~30S: Solis L looks separated independently from the following Ddalia new dark band. The longitude is around 085W. The spc is still not distinct.

  Erratum: We are sorry for an irrecoverable mistake of the date on this image in the printed version of CMO #257 (at p3252): The date should read 28 Jan 2002 (on Don's Birthday).

  On 2 February (320Ls) the DPk images were made at ω=108W & 111 and the area of Solis L reminds us of the singular aspect observed in 1877 (see TROUVELOT's drawing in ANTONIADI's book p138, Fig 79). It will be quite exciting if the aspect continues to be shown in 2003. DPk's images on 3 February (320Ls) are also good at ω=090W (+091W), 095W. Agathodmon with Melas L is visible. Argyre is light near the limb. The spc looks to shine.

  On 26 January (315Ls), Dave MOORE (DMr) in Arizona took images at ω=180W (at 00:54 GMT), and Frank MELILLO (FMl) in NY made an image at ω=139W (at 22:42 GMT) : Both images show M Sirenum. The R image of DMr seems to show a singular split on M Sirenum. The G image shows a light morning continent.
  On 12 February (325Ls)
DMr produced images at ω=017W: The dark band runs as before from M Serpentis to M Erythrum. S Margaritifer is dark evident. Hellas is light near the evening limb.

Observations from Japan:
  The weather was generally poor at Fukui through the period, but just only on 19 January (312Ls) the present writer (
Mn) had a good seeing condition. Mn observed nine times from 5:50 GMT (14:50 JST) at ω=323W to 11:10 GMT at ω=041W: Syrtis Mj was apparent until ω=342W where Libya was white near the limb. Hellas was roundish and slightly of whitish light and was seen until ω=031W. Hellespontus is visible and the shadowy D Hellespontic was separated by a faint area from the spc. The spc was clearly seen round and bright. The dark band in Noachis from M Serpentis was evident. At ω=352W, S Sabus was seen and Margaritifer S was out from the morning mist. The northern desert was reddish. At ω=031W, Niliacus L was seen adjacent to the nph. The temperature inside the dome was down from 7C to 4.
Km) on 19 January (312Ls) produced an composite image at ω=011W: Aram is light and Niliacus L is visible, though S Sabus is unstable. The spc is clear.
Ts) made her last series of observations on 23 January (314Ls) at ω=315W~344W (10:00 GMT): The slim Syrtis Mj and the round Hellas were watched to move from the centre to the east. The spc was checked light. the apparent angular diameter =5.6", and the last drawing was numbered Ts-421D.
Km gave a series of good images on 24 January (315Ls) at ω=300W, 311W, 320W, & 333W: At ω=300W, Syrtis Mj is nearly at the centre and Hellas round. At ω=311W, Zea L is visible inside Hellas. The image at ω=320W is excellent in the sense that the three bands of Hellespontus, the Noachis dark band and S Sabus are separated. Trinacria is light.
Id) observed on 30 January (318Ls) at ω=289W, and on 31 January (319Ls) at ω=272W: Syrtis Mj seems to be seen but the contrast is low. M Hadriacum was checked?

  Km took images on 1 February (319Ls) at ω=230W & 237W where the morning Hesperia is whitish misty. The latter is good and depicts the shadowy area in theria quite large. M Cimmerium was perfect, and M Chronium was quite dark.
Id observed on 3 February (321Ls) at ω=235W, ω=242W, but the seeing was poor because the time was slightly late.
  On 6 February (322Ls),
Km shot at ω=186W (8:46 GMT): Km informed us that the seeing was very poor, but the image composed looks strange in the sense that M Sirenum splits into two and a dark band goes to the south from the preceding area of M Sirenum. At Fukui, Mn watched at ω=183W, but any abnormality of M Sirenum was not checked in particular, while the north of M Sirenum was very bright near the limb (this is shown also in Km's image). A shadowy segment went down northward from the western part of M Sirenum. M Cimmerium showed a tint of brown. From ω=193W, Electris-Eridania looked covered by a morning mist. The eastern limb of the continent zone was also light. The spc was dull. Id watched at ω=210W: The seeing was not very poor, but just M Cimmerium was checked. Mn observed until ω=222W where the morning area of the continent zone was misty.
Mk) could observe on 9 February (324Ls) at ω=156W, and on 10 February (324Ls) at ω=151W & 161W ( the apparent angular diameter being 5.2") and recorded the dark band of M Cimmerium and the brightness of the northern afternoon side.
  At Fukui,
Mn observed on 13 February (326Ls) from ω=114W (to ω=143W) and on 15 February (327Ls) from ω=065W (to ω=123W) and could aim at the area of Solis L. Compared with the definite darkness of the area of Auror S, Solis L was not so vivid, while at ω=094W (just the Sun set), Solis L and the Ddalia band became evident at 600x. The spc was also distinct (at 327Ls) and its preceding limb area was also light. A morning mist to the south of Ddalia.
Km made a composite image on 15 February at ω=087W: Solis L is shown (this is more evident on the image on the following day 16 February at ω=083W to be reported in the next issue). Id observed on 15 February at ω=151W where Solis L remained near the afternoon limb.
Mo) tried several times to produce images; but he could not usually begin earlier and so his most times were after the seeing was broken. However those made on 3 February (320Ls) (Sunday) at ω=226W, and on 9 February (324Ls)(Sat) at ω=190W were rather moderate.

From England:
  We received a set of images of Damian PEACH (
DPc) made on 15 February (325Ls) at 17:45 GMT when the altitude of the planet was high up at 38. The images show the surface at ω=229W, where the spc is distinct though small, and M Cimmerium was shown in contrast with the light continent to its south. The dark area in theria is shot here as a small but very distinct spot. A shadowy area goes down from the west of M Sirenum.

Images Supplemented:
  We further received as follows:

De GROFF, Kent (KGr) Kwajalein, Marshall Is

43 CCD Images (28, 29, 31 May; 2, 4~11, 18~21, 25, 27~30 June;

3~9, 11~15, 26 July 2001)

f/62 25cm F/6.7 spec with Nikon 950

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

1 Set of CCD Images (14/15 November 2001)

f/44 41cm F/6 spec with Lynxx PC

  MARSHALL Islands are located in the Northern Hemisphere but quite near the equator, and so Mars was higher in the height of the season. The Longitude of the Islands is around 170E, so that the KGr's site is ahead of Japan by 2~3 hrs and so precedes us importantly. Don PARKER once forwarded us some crucial images of KGr at the beginning of July, and this time we received a lot of others directly from KGr: A total of 27 images taken after the onset of the global dust storm are now in the CMO-Web. We plan also to upload the former images. KGr secured good images when we were suffering from the rainy season. The image on 19 June shows a white mist over Hesperia that was at the afternoon side, but not yet near the terminator. KGr usually made one composite image on one day, but on 8 July he produced four at ω=091W, 106W,120W,124W & 133W.
DPk sent us a set taken on 15 November (161Ls) at ω=166W where the dark band of M Sirenum and M Cimmerium winds. The spc was quite large yet. The apparent angular diameter =8.1".


HE next report in #258 deals with the observations during a one-month period from 16 February 2002 (328Ls) to 15 March 2002 (342Ls).

Reports will be acknowledged if air-mailed to M MINAMI at Mikuni
(ask the mail-address through vzv03210@nifty.com ) .

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