23

rd Report:

The CMO/OAA Observations made during a fortnight period

from

16 January 2004 (334Ls)

to

15 February 2004 (351Ls)

 


An OAA Mars Section article to be published in CMO #288 (25 February 2004 issue)


Masatsugu MINAMI, Director of the OAA Mars Section


Japanese version here


F

rom this time, we treat one-month period, and here we review the observations made during the period from 16 January 2004 (λ=334Ls) to 15 February 2004 (λ=351Ls) when the apparent diameter δ went down from 7.5" to 6.2". Otherwise the central latitude φ was from 25S to 19S, and the phase angle ι decreased from 41 to 38. The observations made abroad decreased (though Don PARKER (DPk)s activity was still remarkable), but in Japan the observers at the side facing to the Pacific Ocean were active. The areas of the rear side (including Fukui) were however almost always covered by the snowy cloud, and even when the sky was cleared, we had snowfall on the rooftop around the dome. On 22 January it snowed all day long at Mikuni.

However since the sun set earlier and the apparent declination was up from +7.5 to +14.8, we were able to watch nine times every 40 minutes (in the case of the present writer (Mn) he observed on 10 Feb from 15:40 JST to 21:00JST (Mn-1092D)). SIEGEL (ESg) returned from her journey to New Zealand and resumed her observations from 9 February.

 

AKUTSU, Tomio (Ak) Karasuyama, Tochigi, Japan

3 Sets of RGB Images (+1 B +1 IR images)

(18, 26 January; 8, 10 February 2004)

f/3332cm spec with a Bitran BJ-41L

IWASAKI, Tohru (Iw) KitaKyushu, Fukuoka, Japan

22 Drawings (17, 29, 31 January; 9, 10, 12, 15 February 200

40021cm speculum

KUMAMORI, Teruaki (Km) Sakai, Osaka, Japan 

29 CCD Images (20, 21, 24, 27, ~29, 31 January; 4, 5, 8, 11 February 2004)

f/4060cm Cass# with a ToUcam

#Sakai City Observatory

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

3 Red CCD Images (17, 21 January; 5 February 2004)

20cm SCT with a Starlight Xpress MX5

MINAMI, Masatsugu (Mn) Fukui, Fukui, Japan

17 Drawings (31 January; 10 February 2004)

480, 600, 63020cm F/12 ED Goto refractor*

*Fukui City Observatory, Fukui

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

17 Sets of RGB Images (+18 IR images)

(20, 24, 27, ~29, 31 January; 8, 11 February 2004)

25cm spec equipped with an ST-5C

MURAKAMI, Masami (Mk) Yokohama, Kanagawa, Japan

8 Drawings (18, 28 January; 4, 10, 13 February 2004)

320, 40020cm speculum

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

17 Sets of RRGB Images (17, 23, 26 January; 2, 3, 7, 10 February 2004)

f/5941cm F/6 spec equipped with an ST-9XE

PEACH, Damian A (DPc) Loudwater, Buckinghamshire, UK

3 Sets of RGB + 6 LRGB Images (16, 24, 27, 29 January; 8 February 2004)

f/3128cm SCT with ATK-1HS

  

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

1 Set of RGB Images + 3 IR +1 UV Images (29 January; 8, 9 February 2004)

35cm SCT with a modified B&W ToUcam Pro

SIEGEL, Elisabeth (ESg) Malling, Danmark

2 Drawings (9, 11 February 2004)

27020cm F/10 SCT

  

TEICHERT, Grard (GTc) Hattstatt, France

2 Drawings (23 January; 13 February 2004)

33028cm SCT

  

Van der VELDEN, Erwin (EVl) Brisbane, Australia

1 CCD Image (14 February 2004)

f/2923cm SCT with a Vesta Pro modified

WARELL, Johan (JWr) Tcuson, AZ, USA

3 Sets of CCD Images (18, 19, 27 January 2004)

f/2425cm SCT with a ToUcam

 

Aftermath of the Dust Cloud in December: The December 2003 dust was no more active except for the drifting airborne dust. Just PARKER (DPk)s images on 17 Jan (λ=335Ls) at ω=053W, (055W), 059W show Aurorae S as separated as if the neighbourhood looked dusty, and the limb side of Chryse on WARELL (JWr)s images on 18 Jan (λ=335Ls) at ω=084W must have been bright because of the drifting dust. However according to TES, no conspicuous disturbance was known during the period; just several exceptional images were obtained like a slight disturbance near Utopia on 24 Jan (λ=339Ls), but they all looked beyond the terrestrial observations. The inside of Hellas looked still dusty, but Tohru IWASAKI (Iw) noted that the appearance of Hellas on 15 Feb (λ=350Ls) at ω=289W, 299W, 308W suggest the ground-lit.

Hellas: At this period of the season, it has been known, especially from the 1990 observations, that the inside of Hellas shows a light bottom at the northern part and at the western side sometimes affected by condensates (cf CMO #113 (25 Jan 1992 issue) Note (3) p0988). The images of Hellas on PEACH (DPc)s on 16 Jan (λ=335Ls) at ω=323W~332W and DPks on 26 Jan (λ=340Ls) at ω=337W~345W suggest a typical figure. However to pursue the problem of the condensates, observations this period were not enough. The next 2005 apparition may be more appropriate on this point. Just the morning mist or condensate over Hellas was checked by the following observations: PELLIER (CPl)s on 29 Jan (λ=342Ls) at ω=208W, 212W, and DPks on 2 Feb (λ=343Ls) at ω=273W, 279W, and on 3 Feb (λ=344Ls) at ω=263W, 270W. The Hellas area began to face us in Japan from around 5 Feb as is shown by KUMAMORI (Km)s on 5 Feb (λ=345Ls) at ω=357W. On this image Hellas is very bright near the limb, but this must have been due to the large phase angle (ι=40). On 9 Feb (λ=347Ls), and 10 Feb (λ=348Ls) at ω=338W, Iw regarded the evening limb side Hellas as less light than the sp region. One the same day, the present writer (Mn) watched Hellas inside the disk from ω=289W to 328W, and at the limb side from ω=338W to 007W: Inside the disk Hellas was rather dull inside just light at the northern bottom and the western part, and at ω=318W it was as light as the northern deserts, but the latter was rather reddish while Hellas was yellowish. At this point Libya was whitish near the limb, and Hellas became gradually whitish near the limb side; at ω=347W it turned more whitish than the spr. MURAKAMI (Mk) already saw Hellas bright at ω=300W. ι=38. AKUTSU (Ak)s B at ω=356W does not however show Hellas. On 11 Feb (λ=348Ls), Km and MORITA (Mo) produced ccd images of the inside of Hellas: Mos B at ω=326W does not show the white matter.

 

Mare Serpentis: The area of M Serpentis and the eastern part of Deucalionis R has been an interesting area to be watched because the swept out of the ground sand over there were apparent ever since July 2003. Mo took an image on 8 Feb (λ=346Ls) at ω=330W, and this, though ι was quite large 39, should be added to the ω=328W series images presented in

http://www.kwasan.kyoto-u.ac.jp/~cmo/cmomk/2003/M_Serpentis_June_Nov.jpg .

Mns observations on 10 Feb (λ=348Ls) at ω=309W, 318W, 328W, 338W also show the similar aspect. Just as shown also by Iw on 12 Feb (λ=349Ls) at ω=318W, 328W, 348W, the eastern part of Deucalionis R looked lighter than before. By ccd DPks images 26 Jan (λ=340Ls) at ω=337W, 340W, 345W show the area to be more contrasty than before. DPcs LRGB image on 16 Jan (λ=335Ls) at ω=332W also suggest the fact. On DPks image on 23 Jan (λ=338Ls) at ω=010W~017W, the area of M Serpentis was already near the limb, while show well the region of Noachis: the dark band crossing Noachis from M Serpentis looks irregular and incomplete, but making a long band.

 

The SPC and SPH: As previously noted, the residual spc was explicitly shown by DPc on 18 Dec (λ=318Ls,, ι=42) at ω=239W~263W. Here DPk claims that his images on 17 Jan (λ=335Ls) at ω=053W, (055W), 059W show the final or residual stage of the spc, and it was apparent visually to him at magnification 700. On 28 Jan (λ=341Ls) at ω=090W, 100W, Mk noted that the spr was largely light. Kms image on 29 Jan (λ=341Ls) at ω=066W also show the light area. On the same day, Iw noted at ω=095W, 105W, 115W, 124W that the light area looked like a misty hood. The afore-cited CPl B images, made on 29 Jan (λ=342Ls) at ω=212W, may also show partly a condensate haunting at the spr. On 31 Jan (λ=343Ls), Iw however commented that it was delicate it was a hood or just misted based on his observations at ω=076W, 085W, 095W, 105W. On the day, Mn saw a dully bright spot (just like the spc) at ω=046W and 075W but admitted that it was natural to regard the spr as governed by the condensate. Mos B image on the day at ω=054W seems to show a light mist at the spr. DPks images on 10 Feb (λ=348Ls) at ω=194W and 197W show more clearly the hood-like matter. From another hemisphere, Mk, Iw and Mn noted on the day (10 Feb) that the spr coupled with the evening Hellas was covered by the white condensate (though Int). On 11 Feb (λ=348Ls) at ω=076W, ESg saw a light area through Int, but noted that it was not seen through her favourite Wr#47.

 

The Argyre Condensates: The Morning condensate is apparently seen on the B images taken by DPk on 23 Jan (λ=338Ls) at ω=017W and on 26 Jan (λ=340Ls) at ω=339W, 345W. On 29 Jan (λ=341Ls), Iw visually observed it at ω=095W. However as Argyre moved on to the afternoon side, Argyre showed its triangle ground area as shown by DPk on 17/18 Jan (λ=335Ls) at ω=055W, 059W, and by Km on 29 Jan (λ=341Ls) at ω=050W~077W, and by Mo on 31 Jan (λ=343Ls) at ω=053W, 063Wand so on. On the other hand at the evening limb, ESg recorded Argyre was very bright through Int (also bright throughWr#47) on 9 Feb (λ=347Ls) at ω=101W.

 


T

he next issue shall treat the observations made during the one-month period from 16 February 2004 (λ=351Ls) to 15 March 2004 (λ=005Ls, δ=5.3").


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