1998/99 Mars Observation Reports -- #09--

OAA MARS SECTION

CMO Fortnight Report
published in CMO #216 (25 April 1999)
Martian Surfaces in the First Half of April 1999
from 1 April 1999 (118degsLs) to 15 April 1999 (125degsLs)

  We received the observations submitted to the CMO this period as follows:

      AKUTSU, Tomio (Ak)   Karasuyama, Tochigi, Japan
            13 CCD Images (4, 5, 8, 9 March 1999) f/60 32cm spec equipped with a Teleris 2 

      FALSARELLA, Nelson (NFl) Rio Preto, Brasil
            18 Drawings (17, 19, 25, 27~31 March; 2~7, 8/9, 10, 11, 12 April) 
                                               260, 325x 20cm speculum

      GRAY, David  (DGr)   Kirk Merrington, Durham, UK
             5 Drawings (28 March; 1/2, 6/7 April 1999)    350x 42cm Dall-Kirkham

      HERNANDEZ, Carlos  (CHr)  Miami, FL, USA
             2 Drawings  (13 April 1999)  235-285x 20cm SCT

      HIGA, Yasunobu (Hg)  Naha, Okinawa, Japan  
            32 Video Images (6, 7, 8, 13, 14, 15 April 1999) 
                                     25cm speculum equipped with Sony DCR-TRV900 

      ISHADOH, Hiroshi  (Id) Naha, Okinawa, Japan
            13 Drawings (5, 7, 8, 13, 14, 15 April 1999)  400, 500x 31cm speculum

      IWASAKI, Tohru (Iw)  Kitakyushu, Fukuoka, Japan
             9 Drawings (2, 4, 7 April 1999)  400x 21cm speculum

      MELILLO, Frank J  (FMl)   NY, USA
             6 CCD Images (11, 14 April 1999) 20cm SC  Starlight Xpress MX-5
 
      MINAMI, Masatsugu (Mn)   Fukui, Japan
            49 Drawings (1, 3, 4, 5, 14, 15 April 1999)  400x 20cm refractor* 

      MURAKAMI, Masami (Mk)   Fujisawa, Kanagawa, Japan
            21 Drawings (5, 6, 7, 8, 9, 13, 14 April 1999)  320, 425x 20cm Saheki speculum

      NAKAJIMA, Takashi  (Nj)  Fukui, Japan
            26 Drawings (3, 4, 5, 8, 12, 14, 15 April 1999)  400x 20cm refractor*

      NARITA, Hiroshi  (Nr)  Kawasaki, Kanagawa, Japan
             8 Drawings  (4, 5, 8, 13, 14, 15 April 1999)   400x 20cm refractor

      NIKOLAI, Andre  (ANk)   Berlin, Deutschland
             2 Sets of CCD Image  (1/2 April 1999)   15cm Refraktor am WFS

      PARKER, Donald C  (DPk)  Miami, FL, USA
             9 Sets of CCD Images (1, 2, 3, 6, 15 April 1999) 
                                     f/55 41cm speculum equipped with a Lynxx PC

      SCHMUDE, Richard W, Jr (RSc) GA, USA
             1 Drawing  (2 April 1999)  380x 25cm speculum

      SIEGEL, Elisabeth (ESg)  Malling, Danmark
             1 Drawing  (1/2 April 1999)  270x 20cm Schmidt-Cassegrain

      TEICHERT, Gerard  (GTc) Hattstatt, France
             2 Drawings  (1, 10 April 1999)  310,330x 28cm Schmidt-Cassegrain

      WARELL, Johan  (JWr)  Uppsala, Sweden
             4 Drawings  (31/1, 1/2, 2/3, 4/5 April 1999) 
                               25x 10cm SC,  180x 30cm SC, 330x 16cm refractor
       
                                               * Fukui City Observatory

  Tripod Observations:

  Anybody will soon recognise that the location of Japan is important from the viewpoint of a global observations of the Martian surfaces. Let us pick out the case of 6 April this time: Don PARKER at Miami obtained on 6 April good images during the period from 05:45GMT to 06:00GMT (nearly at LCM=026degW), and so the early morning counted in GMT must have been watched by the American observers. The European observers are to observe at midnight in GMT.In fact David GRAY made his first drawing on the day at 23:40GMT (LCM=284degW). Then how about the day time in GMT? Mars needs to be watched whole day through, and the Japanese observers can contribute in this point. For example, on 6 April, HIGA (Hg) at Okinawa watched the planet from 15:35GMT to 18:56GMT (from LCM=167degW to LCM=216degW), and we may extend the time span from 10:00GMT to 18:00GMT soon. Thus our observations relay the American observations to Europe. If more detailed, Hawaii is also a relay point from the American continents to the Far East areas. There is another important relay point in Brasil which is located between Europe and the North America from the viewpoint of longitudes.

  American Observations:

  ( As stated, Brasil where Nelson FALSARELLA (NFl) works is an important observing site to the extent that NFl's observations will relay the European observations to the US observers. For example, on 2 April Don PARKER started from 5:30GMT, and R SCHMUDE (RSc) observed at circa 6:00GMT, while Elisabeth SIEGEL observed at 00:00GMT. NFl worked on the day halfway at 3:00GMT showing that the location of NFl is a divide. Theoretically good, but it seems that NFl observes earlier than his own time: In fact on 8/9 April he observed at 00:00GMT and so is like an European. On 5 April he observed at the same time as Johan WARELL in Sweden at 01:00GMT. Furthermore on 10 April NFl was watching at 0:55GMT when G TEICHERT in Rhineland observed. On the other hand no observation of NFl which competes with the US observations, and hence we treat here the case of NFl together with the European observations below. )

  On 1 Apr (118degLs), PARKER (DPK) tried to shoot the planet, against the windy condition, to check the phenomenon recorded by HERNANDEZ (CHr) the day before (cf #215). DPK only used RG610 and Int light at LCM=060degW and 071degW. These images are detailed showing the dusty white cloud at the offing of Aromatum Pr, and also Hyperboreus L together with Iaxartes, but recording no anomaly.

  On 2 Apr (119degLs), DPK made images at LCM=056degW and 079degW, both of which show a white canopy to the south of Solis L. The former image shows the large area of M Erythraeum and Margaritifer S to Aurorae S shows a mixing of a densely reddish colour. This image shows clearly Iuventae F. On the B part of the latter image, Ascraeus L is quite dark. Opir is now white (while the place was just ground lit even if the clouds floated in the Northern Equatorial Band). On the same day (2 Apr), RSc observed at LCM=065degW after a long absence. The S limb was covered by a cloud. The evening mist crept up to Xanthe.
Don PARKER's Blue Image
on 2 April 1999(118degsLs)
at LCM=078degW

  On 3 Apr (119degLs), DPK worked at LCM=055degW and 071degW. The R images are very detailed. The extension of Orestes is apparent. The B image at LCM=071degW seems to show the Ascraeus cloud in addition to Ascraeus L which is very dark. The R image may convey a few of Montes.

  On 6 Apr (120degLs) DPK obtained a good image around at LCM=026degW. The inside of M Acidalium is shot very detailed. The Orestes extension is certain, and Chasma Boreale is also seen.

  On 11 Apr (122degLs) MELILLO (FMl) produced a Red CCD image at LCM=338degW, and then took a sequence of B images up to LCM=001degW by the use of Wr47. The setting of Hellas and the in creasing of the Chryse mist are well shown. The Libya mist is also shown.

  On 13 Apr (124degLs), HERNANDEZ (CHr) drew by use of Wr23A at LCM=290degW and by use of Wr38A at LCM=303degW: Syrtis Mj was near the CM, but M Acidalium was already inside finely, and CHr detailed the area from Protonilus to Utopia.

  On 14 Apr (124degLs) at LCM=299degW, FMl took a CCD image by Wr25. The B images are from LCM=301degW to LCM=309degW: Hellas bright, Syrtis Mj is apparent on its southern part (densely reddish). The phase angle=9deg.

  On 15 Apr (125degLs), DPK obtained images near at LCM=281degW and 304degW: In the former, Elysium is white near the terminator, and in the latter S Meridiani is coming in. The inside of Hellas is not uniform, but a fourth is less bright in the west part. In R, the top looks caved in.

  Observation from Japan:

  At the beginning of April, they observed Aurorae S and its east in the US, but in Japan we watched its far west at around Olympus Mons. For example, on 1 April at Fukui we observed from LCM=181degW to LCM=250degW (by MINAMI (Mn)), while on 15 April we watched from LCM=042degW to LCM=145degW (by NAKAJIMA (Nj)): That is, we were able to watch the surface from LCM=040degW westward to LCM=250degW during the present period. The halfway area at around LCM=140degW was repeatedly observed, and so every time Olympus Mons played the part. The observation time went from 12:30GMT to 19:50 GMT with the planet at meridian near 16:00 GMT. This implies there was a large time difference from America, while our last session was carried out in the evening in GMT so that our observations will soon approach the European earlier observations.

  On 1 Apr (118degLs), Olympus Mons was observed very bright near at the terminator, and then disappeared. At LCM=220degW, only an afterimage was seen (phase angle=18deg). On the day Syrtis Mj was witnessed at LCM=217degW, and it showed a light blue up until LCM=250degW beneath the morning mist. Elysium and Cebrenia made a Y shaped light region, but Elysium was as white as the evening mist and whiter than Cebrenia at LCM=240degW. At LCM=250degW, Elysium was covered by the evening mist. The white part in Elysium looked rather small, and may be a cloud covering Elysium Mons.

  On 2 Apr (119degLs), IWASAKI (Iw) observed: At LCM=221degW, he only saw the morning mist only, but it appeared weakly at LCM=321degW. He detected a small bright spot inside Elysium in the former, but soon lost it. At LCM=240degW, Iw saw the morning Hellas.

  On 3 Apr (119degLs), the present writer (Mn) was aware of the cloud at Elysium Mons in Elysium at LCM=224degW et al. Elysium was surrounded by a rather ring-like dark band: Cerberus was curved as well as Phlegra. The west side was thickly bounded by the Aetheria dark patch which is densely reddish. At LCM=268degW, the curve of Cerberus and Phlegra was still seen.

  On 4 Apr (119degLs), the Asuwa-Yama (a hill, only 100 meters a s l) where the Fukui City Observatory is located has become full of cherry blossoms illuminated by a lot of lanterns: the temperature was 10 degrees C on the night. At LCM=164degW, a dark band preceded Olympus Mons and at the same time the Tharsis bright area was divided into two, upper and lower. We had a preferable seeing at LCM=184degW, and saw Propontis I to show a brownish tint. The Aetheria dark patch was still underneath the morning mist and the southern part of the patch was bluish. Near the npc, Olympia was detected. At the opposite southern limb, there was a bright fine part to the south of the east part of M Cimmerium which was brighter than Olympus Mons through an O56 filter. Olympus Mons was very white, and according to Nj, it was out standing though quite soft at LCM=198degW, and still visible at LCM=215degW, but became very fainter at LCM=218degW (since phase angle 16deg, the local time was 6:50 pm). Iw also watched Olympus Mons from LCM=193degW (distinct and brighter than the npc) to LCM=213degW (weaker image). His description of the Aetheria dark patch at LCM=193degW was realistic. He distinguished three ingredients inside M Cimmerium. The morning mist was invading Elysium. The present writer saw the day some details insides of M Cimmerium at LCM=213degW. Syrtis Mj showed up to him at LCM=212degW. Nj saw Syrtis Mj at LCM=218degW, and separated Hesperia. Elysium looked closed by roundish dark ring. AKUTSU (Ak) took several CCD images at LCM=147degW and at LCM=182degW: The latter is a good image and shows Propontis I and the Aetheria dark patch. Olympus Mons is also visible in R. Elysium is whitish at the morning side.

  On 5 Apr (120degLs), a considerable number of observations were obtained. Ak took CCD images of LCM=152degW and LCM=163degW; the former showing Olympus Mons isolated in G, and the latter showing vaguely Propontis I. MURAKAMI (Mk) chased Olympus Mons from LCM=150degW to LCM=180degW. ISHADOH (Id) observed at LCM=196degW and at LCM=206degW: The latter shows a faint N Alcyonius near the morning limb, and detected Olympia. Elysium seemed to have just become light. Nj regarded Elysium ground lit at LCM=223degW. Mn's observations on the day were as follows: At LCM=164degW, as the day before, the Tharsis cloud looked divide to the southern and northern parts. At LCM=175degW, M Sirenum appeared greenish at the evening side. On the other hand, the northern part of the Aetheria was brownish but its southern part was bluish beneath the morning mist. The intensity estimates at LCM=194degW: Olympus Mons 0.0, the npc 0.5 (Olympia was weaker), the morning mist 1.0~1.5, Elysium 2.0, the bright segment at the southern limb 1.5 et al. This bright segment was seen at LCM=184degW as before. At LCM=204degW the northern part of Phlegra was pretty curved. Hellas was found to have appeared at LCM=214degW. Mn was then to be absent from observation until 14 Apr.

  On 6 Apr (120degLs), HIGA (Hg) used his favourite Video camera from LCM=167degW to LCM=216degW. From the outset Olympus Mons is isolated. At LCM=177degW, the dark band preceding Olympus Mons is evident. Olympus Mons began to shine from LCM=186degW. Elysium is light inside the morning mist. At LCM=216degW, Elysium (maybe Mons) is small light even in B (animation). The morning mist is thick.

  On 7 Apr (121degLs), Mk started from LCM=125degW, and caught the isolated Olympus Mons at LCM=145degW (according to his calculation the local Martian time was 1:40 pm). Id saw the smaller and whiter Elysium Mons at LCM=223degW and 232degW. Iw and Hg intervened between Mk and Id: Iw observed at LCM=167degW, 176degW, and 186degW; the first two detecting Olympus Mons and the dark band following Tharsis ridges. Tharsis brighter. Hg took the Video images from LCM=152degW (15:10GMT) to LCM=199degW: at LCM=152degW the image shows the dark band between Olympus Mons and Tharsis. At LCM=162degW, the Tharsis cloud proves to consists of two part, the lower being whitish, but the upper one off-white. The lower one must be connected with Ascraeus Mons. At LCM=191degW, the Aetheria dark patch is under is seen through the morning mist. At LCM=198degW, there seems to exist a light spot in Zephyria, but not visible in B.

  On 8 Apr (122degLs), Ak took by CCD the area of Solis L at LCM=111degW where the southern limb looks hazed. At LCM=127degW, the white band from Xanthe to Olympus M is apparent; the latter being isolated and the dark band between evident in B. At LCM=153degW, Olympus Mons shines. Nj at Fukui also pointed out that the evening limb was bright from Tharsis to the far south at LCM=131degW~LCM=141degW. In particular Mk was puzzled with the presence of a blue whitish matter at the SE limb at LCM=131degW. at the same time, Mk (as well as Nj) isolated Olympus Mons whose local time was 0:45pm according to his calculation.

  On 9 Apr (122degLs) Mk again noticed the blue whitish cloud at the SE limb (maybe at Thaumasia Foelix) at LCM=122degW and chased it upto LCM=142degW, while it sank out by LCM=150degW. Since the cloud rotated, it was considered no polar hood, (and so he called up Mn at Otsu the next day and was advised to ask other Japanese observers by email). The seeing the day at the Kantoh district seemed to be good, and Mk otherwise recognised the faintly shining Olympus Mons at LCM=122degW (at 0:05pm LMT) as well as Ascraeus Mons at LCM=132degW (2:40pm LMT). Olympia was also evident to him. Fortunately on the same day Ak pointed his Teleris 2 to Mars at LCM=095degW, 115degW, 128degW, 137degW, 151degW and 163degW: The last one being the best with Propontis I inside and Olympus Mons following a dark band in G. The image at LCM=137degW is also impressive where Xanthe is still very bright. Ak processed the images by Mk's request in a hurry, and in fact the image at LCM=095degW proved the white cloud to the south of Solis L. The sky was unfavourable for a while.

(left) MURAKAMI's drawing on 9 Apr 1999 (122degLs) at LCM=132degW
(right) ISHADOH's drawing on 13 Apr 1999 (124degLs) at LCM=133degW

  On 13 Apr (124degLs), there were obtained many good observations. Mk observed at LCM=089degW, 099degW, 109degW, 119degW & 129degW. The first observation showed him the pale pall at the S limb, while it passed the CM at around LCM=109degW. The evening haze was thick, and there were several cloud patch along the Equatorial Band to make an EBC. At LCM=128degW, Alba became light. Hg's Video recorder worked from LCM=068degW to LCM=111degW: At LCM=077degW, the Mk white cloud to the south of Solis L, and the morning mist thick. At LCM=106degW, Olympus Mons looks well separated from Ascraeus Mons. The morning side appears interesting (to be discussed in a coming meeting). Id observed under a favourable seeing condition at LCM=123degW, 133degW, 143degW and 152degW: At LCM=123degW, he observed the cloud noticed by Mk to be downward to Daedalia. Phoenics L was evident to him. Ascraeus Mons was roundish obvious in addition to Olympus Mons and Alba. Olympia apparent. The drawing at LCM=133degW is cited here: Pavonis Mons was clouded, while Id regarded Arsia Mons as nearly cloud free. At LCM=152degW, the Tharsis-Xanthe cloud became very complexed.

  On 14 Apr (124degLs), Mk observed at LCM=076degW, LCM=085degW, LCM=095degW and LCM=105degW. Hg shot from LCM=093degW to LCM=141degW. Id observed at LCM=149degW: Mk saw an indefinite EBM at LCM=076degW, and saw the Thaumasia cloud come down to Daedalia at LCM=095degW when Aurorae S was fainter near at the terminator with a bright opir. The images of Hg show already the white Olympus Mons at LCM=121degW. Olympia is evident at LCM=131degW. The image at LCM=141degW is excellent. Mn returned home and observed at Fukui at LCM=061degW, and then from LCM=105degW to LCM=144degW every 40 minutes. At LCM=105degW, he noticed the Mk pall, and saw it go downward to Daedalia at LCM=115degW and 124degW. Nj also confirmed the motion of the Cloud at LCM=120degW. Nj depicted Ascraeus Mons , Olympus Mons and the dark band which separated the two at LCM=129degW and 139degW. Mn checked Olympia from LCM=115degW, and endowed with a moderate seeing at LCM=134degW, clearly saw it. At LCM=115degW he noticed a bright area which was suspected to be the Ascraeus Cloud, but already at LCM=124degW Olympus Mons showed up.

  On 15 Apr (124degLs), as was aforementioned, at Fukui we observed from LCM=042degW to LCM=145degW during which Hg observed from LCM=057degW to LCM=102degW and Id did, annoyed by clouds and smokes, at LCM=059degW, 091degW, and 125degW: Hg's images became good from LCM=077degW when Hyperboreus L is evident, and at LCM=096degW, the Ascraeus-Cloud-like area is found (to be discussed). Id watched the S limb cloud to the south of Solis L at LCM=091degW where Opir was lit. Hyperboreus L was connected with M Acidalium. At LCM=125degW, Id noted Olympia near the npc, and Olympus Mons before the CM. The Thaumasia cloud was downward to Daedalia. Nj watched the Mk cloud at LCM=116degW. Mn's observations were as follows: at LCM=042degW, Hyperboreus L was evident. The morning mist was thicker than the evening one. At LCM=071degW, Ascraeus Lacus was dark and maybe the Ascraeus Cloud seemed to be present. The evening mist looked condensed at LCM=082degW. At LCM=121degW, the seeing improved, and Olympus Mons was witnessed at about 11:45 am LMT as well as Ascraeus Mons. Towards north, Olympia was obvious. From this angle the Mk pall was at the opposite of the npc just like a canopy, but the core was already in the afternoon side. At LCM=130degW, Ascraeus Mons was more roundish evident, but not yet so whitish (2:20 pm MLT).

  From Europe and Brasil, they observed as follows:

  On 1 Apr (118degLs), TEICHERT (GTc) observed at LCM=017degW and WARELL (JWr) did at LCM=028degW: Both show M Acidalium near the CM. In former Tempe is a whitish place, while the latter shows the morning and the evening mist.

  On 1/2 Apr (118degLs) GRAY (DGr) observed at LCM=322degW and at LCM=338degW while SIEGEL (ESg) did at LCM=334degW. DGr used Wr25 for the former, and Wr58 for the latter. Hellas was bright but elusive by LCM=332degW, but by the use of the G filter it was seen invading down to Syrtis Mj. Chryse became striking by LCM=324degW in R. DGr considers that the np area still hazed due to a G appearance. ESg also checked the bright Chryse morning mist. She also saw an evening mist at the southern part of Syrtis Mj (she considers that the place might be Iapygia Viridis). Andre NIKOLAI (ANk) took on the same day some CCD images especially at LCM=339degW and at LCM=347degW: The colour images are the composites of R and B images (see LtE): In the former Hellas is a bit seen, and Chryse morning mist is striking, while in the latter the mist is weakened and M Acidalium shows up in a good form. It is however difficult to see the side near the terminator. On the same day JWr made a further drawing at LCM=002degW by the use of a 10cm SCT: the seeing was so good that JWr detected Nilokeras. FALSARELLA (NFl) in Brasil observed succeedingly at LCM=015degW. The remaining evening mist from Libya was at intensity 1.4 (while the npc 0).

  On 2/3 Apr (119degLs), JWr observed at LCM=313degW where the morning mist is distinct at Thymiamata, and the Libya mist also remained. NFl observed at LCM=350degW that the Libya mist invaded Syrtis Mj.

  On 4 Apr (119degLs), NFl saw an evening mist to the north of S Sabaeus at LCM=355degW.

  On 5 Apr (120degLs), JWr obtained a nice drawing at LCM=322degW: Hellas bright, and there was an evening mist from Libya to Aeria. Syrtis Mj showed a broad and dark northern bottom. The southern limb to the south of Noachis was at intensity 3. The morning mist 2. The npc has a fine dark fringe. NFl observed at LCM=340degW: The northern end of Syrtis Mj is faded to be blue. Hellas at intensity 0.3.

  On 6 Apr (120degLs), NFl observed similarly at LCM=340degW. NFl adheres to the blue Syrtis near the terminator, but theoretically Syrtis Mj looks more bluish seen through the white mist at the limb side than the terminator side.

  On 6/7 Apr (121degLs), DGr observed at LCM=284degW (in B) and at LCM=295degW (in R): Transparency was excellent that night as well as seeing, DGr saw Syrtis Mj to Utopia by the use of Wr47B, while in Wr47, the northern part of Syrtis Mj and Utopia were invisible.The phase angle=14deg. In R, DGr detected several dark spots inside Syrtis Mj including the Huygens crater. NFl observed at LCM=305degW where Hellas was at intensity 0.
  On 8 Apr (121degLs), NFl at LCM=260degW with Hellas 0 and the white Elysium 0.8.

  On 10 Apr (122degLs), NFl watched similarly at LCM=270degW. There was seen a large evening mist which include Elysium. S Sabaeus was coming. GTc observed at LCM=277degW where Hellas was bright and the npc was unrealistically very tiny.

  On 11 Apr (123degLs), NFl at LCM=285degW: the evening mist was similar to the one observed the day before.

  On 12 Apr (123degLs), NFl at LCM=255degW: the mouth of Hesperia was shown. The dark patch at Aetheria (3.8) was drawn.

  We may say NFl should extend his observation time to much later to be connected with the observations in the US: Compare with FMl's time which was over LCM=300degW on 11 and 14 Apr.

  We-Further-Received:

  FALSARELLA's observations made at the latter half of March go as follows: On 17 Mar (111degLs) NFl detected Olympus Mons and the preceding dark band at LCM=147degW~155degW. On 19 Mar, he caught them more inside. On 25 Mar at LCM=070degW, Solis L was seen, but the drawing is not realistic. On 28 Mar he observed at LCM=050degW. 29 Mar (117degLs) and 30 Mar, M Acidalium was near the CM. On 31 Mar (117degLs) the drawing made at c.LCM=000degW: Libya mist and the morning mist were shown.

  GRAY (DGr) also made an observation on 28 Mar (116degLs) at LCM=025degW in R: Aurorae S was dark enough, and Iuventae F was detected. The fine structure of M Acidalium was evident. Hyperboreus L was easily caught dark.