ALPHONSUS as Kozyrev (1958) and Hall (1964) would have seen.

by Lena, Salimbeni, Pau, Crandall

visual observers: Lena and Salimbeni
Images: KC Pau and E. Crandall

Introduction
It was interesting to see the crater as Kozyrev (1958) and Hall (1964) would have seen.

We are talked about two TLP summarized as follows:

2003-Oct-16/17 22:54-23:59 64% Alphonsus_Hall 1964-Oct-27

Alphonsus 1964 Oct 27 UTC 05:18-06:10 Observed by Hall, Johnson, Weresulk (Pt. Tobacco, MD, USA, 16" reflector x400, S=5-7). "Red spot. Pink glow detected with Trident MB & seen visually too." NASA catalog weight=5. NASA catalog ID #863.

2003-Oct-16/17 22:58-01:41 63% Alphonsus1_Kozyrev 1958-Nov-03

Alphonsus 1958 Nov 03 UTC 00:00-01:00 Observed by Kozyrev, Ezerski (Pulkova Observatory, Crimea, Ukraine, 50" reflector, 23A/mm spectrograph) "C.p. redder than rest; emiss. spect. in 4756A, 4100, 3950A (C3), 5165, 5130A (Swann bands) 3 spect. over 3.5 h. Image of c.p. weakened in viol. light on spect. Noted visual decrease in brightness & reddish glow. Decrease in bright, & unnusual white color(at 0300h-0330h). Sudden decrease in vis. bright. Spect. started -- gave norm. Spect. (0330-0340h), conditions almost identical to Alter's on Oct. 26, 1956. Nothing seen on Nov. 2-3" NASA catalog weight=5 (very high). NASA catalog ID #703.

GLR members observed alphonsus on 16 october 2003 from 21:10 Ut to 21:39 UT on 17 october 2003. We reported nothing unusual.Unfortunately clouds were present for many GLR observers.
There was no brightening of central peak nor were any other anomalies seen in the general area.
Negative reports were also obtained by BAA.

ALBEDO VARIATION

The observations of Alphonsus also included monitoring the crater for any abnormal albedo variance. The crater’s albedo was compared with other craters. This technique is similar to what variable star observers use when comparing the brightness variation of a particular variable star.

Lena and Salimbeni reported albedo values using the Elger scale.
Pau and Crandall reported images on Alphonsus.
For each observation , the local altitude of the Sun and his co-longitude, were calculated with the ALPO TOOLS software.

Lena made preliminary observations on daily basis. Lena was able to study the area in a systematic way for any anomaly on 11 october (19:25 UT), 12 october (20:00 UT) and 14 october (4:10 UT). Abedo values are reported using the Elger scale , seeing was II Antoniadi scale (telescope refractor 10 cm f/15 and Newtonian 114 f/8)

features col 104.5 col 116.9 col 133.2

floor Alphonsus 5 4.5 4.5

central peak 7 7 7.5

Dark hal. 1.5 1.5 1.5

bright spots 6 6 6
(smallcraters
G, GA, GB etc...)

MOON BLINK

No significant blink was observed in Alphonsus. Using a W80A and W25 filters, Lena visually estimated the dark haloes (DH) and surrounding floor as more red. In the blue filter DH appeared as darker .
The floor and central peak appears more red.

PRELIMINARY OBSERVATIONS

These preliminary observations served as range finders to fine- tune for the target date of 16 -17 October 2003.

Figure below shows a drawing by Lena (under a High solar altitude ; 11 october 2003 at 19:25 UT).

On 16 october 2003 at 10:32 UT Crandall made an image of Alphonsus (below):

RESULTS ON 16 october -17 october as forKozyrev (1958) and Hall (1964)

Salimbeni observed from 21:10 to 21:30 UT on 16 october 2003. He finished observations due to clouds.
Estimated values are reported below

features 21:10 UT 21:20 UT 21:30 UT

floor Alphonsus 4 4 4

central peak 8 7.5 (§) 8

Dark hal. 1.5 1.5 1.5

(§)= possible effect due to seeing unrelated to other effects

Lena observed from 21:40 on 16 october to 00:15 UT 2003. He finished observations due to clouds.
As for Salimbeni's report the c.p appeared sometimes fluctuate in albedo. It was thought at first that it was an effect of our eyes, but later realized that it was due to the oscillation of the seeing.

Lena was able to report albedo values versus average seeing (below ):

features 21:40 UT 21:55 UT 22:15 UT 22:30UT 23:10UT 23:30UT 00:10 UT

seeing (Antoniadi) III III III/II II II II II
floor Alphonsus 4 4 4 4 4 4 4

central peak 6.5 (§) 6 (§) 6.5 (§) 7.5 7.5 7.5 7.5

Dark hal. 1.5 1.5 1.5 1.5 1.5 1.5 1.5

(§)= possible effect due to seeing unrelated to other effects

so the variation of the Albedo in central peak is related to seeing , thought seeing doesn't affect the darker floor and 3 DH spots.

Pau imaged Alphonsus on 16 october 2003 at 21:31 UT (colong. 166°) using a Newton 25 cm f/6.

Pau imaged Alphonsus on 17 october 2003 at 21:39 UT (colong. 178°) using a Newton 25 cm f/6.

The images showed nothing unusual . We compared images with preceding images taken under similar solar altitude (i.e 17 september 2003 at 21:37 UT colong 172°)
No anomaly was detected (figure below) but it is inters

Conclusion
There was no brightening of central peak nor were any other anomalies seen in the general area.
It was interesting to see the crater as Kozyrev (1958) and Hall (1964) would have seen.

Active international cooperations by individuals making regular systematic, simultaneous observations of the Lunar features continues to be our prime objective.