Lunar Impacts Research
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| − | [[Image:Earthshine f3,3 mio.png|center|640x400px|Earthshine f3,3 mio.png]] Fig.4 - image of earthshine West edge take with telescope Celestron C8 at f/3,3 and always with ASI 120MM by Antonio Mercatali (LI)<br> | + | [[Image:Earthshine f3,3 mio.png|center|640x400px|Earthshine f3,3 mio.png]] Fig.4 - image of earthshine West edge take with telescope Celestron C8 at f/3,3 and always with ASI 120MM by Antonio Mercatali (LI)<br> |
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Versione delle 19:10, 16 giu 2015
The Research, Observation and Recording of Lunar Impacts
This is new programme that has been started by the Lunar Section Research of Unione Astrofili Italiani (UAI), and consists of monitoring the Moon’s night side for Impact flashes that occur when meteoroids, in the Solar System, strike the lunar surface at high velocity. The research on Lunar Impacts started only recently, when on November 18, 1999, the orbit of the Earth-Moon system intersected the Leonids meteor shower orbit. On that date, Brian Cudnik was the first person to observe this phenomena visually, through his telescope, i.e. the flash of light when one object in the solar system collides with the surface of another, and this event was confirmed, and recorded on video, by other independent lunar observers. After this first impact flash, there followed in succession six other impact flashes, always confirmed by independent observers, and this opened up a new scientific way to carry out research into impact rates on our natural satellite. This type of programme is important scientifically for a number of reasons, for example if we measure the brightness of the flash and compare it to that of stars near to the limb of the Moon, then we can obtain the magnitude of the flash, and from this determine the emitted energy of the impact. If the meteoroid is from a known shower, and of known velocity, then its mass can be calculated too.
This study can be very useful in detemining the quantity of “minor bodies” that pass near to the Earth, and to calibrate this with other methods, for example meteor/meteorite rates detected in the Earth’s atmosphere. The programme could have a really important scientific significance for future lunar exploration too, i.e. to be able to know the present day lunar impact rate and how this varies across the lunar surface would be essential to know about in the design of future lunar bases, and also where they should be situated, in order to minimize impact damage.
The mass of meteoroids that fall on lunar surface can vary between some tens of grams and many hundreds of kilograms, while the velocity of impact is between 20 and 72 km/second. These meteoroids can originate from cometary showers that periodically cross the orbit of the Earth-Moon system, or from asteroidal bodies that are more sporadic in nature, and it is this second case that the mass of meteoroids have more significance to the safe design of lunar bases. In the instance immediately after an impact, less than one percent of the total kinetic energy released from the impact, is transformed into visible light that Earth based observers can see in the form of short flashes. These flashes can last from typically less than 1/10th of a second to very occasionally a few seconds for the largest bodies to hit the Moon. After the impact the meteoroid disintegrates and a new, metre scale, crater forms.
The UAI Lunar Section undertakes this research programme in collaboration with the NASA Marshall Space Flight Center who, at professional level, catalogue all observations of Lunar Impacts provided by lunar observers sparse in all the world. Another collaboration has also been started with the Lunar Section’s of British Astronomical Association (BAA) and the american Association Lunar & Planetary Observer (ALPO).
The UAI Lunar Section had collaboration, in the period November 2013 – April 2014, with NASA's LADEE mission (Lunar Atmosphere and Dust Environment Explorer) for research into Lunar Impacts. Although this american spacecraft, developed in the NASA’s Research Center of Ames, CA, could not detect impact flashes directly, LADEE’s LDEX instrument was able to detect the possible presence of dust in lunar exosphere. So by comparing impact flashes, detected by Earth-based astronomers, with dust levels in the exosphere, theoretical models of lunar impact lofted dust can be tested/improved.
Fig.1 - Take of East edge after the phase of Last Quarter Fig.2 - Take of West edge after the phase of New Moon
The ideal instrumentation for the research of Lunar Impacts is a telescope with a motorized mount (both axes) that can to follow the Moon as perfectly as possible (where it is possible to select tracking rate at lunar velocity). The telescope aperture should have a diameter of at least 8”, with a small focal ratio, e.g. f/5 or f/3.3, - this is to enable a sufficiently large lunar field of view, (Fig.3 e 4) and at the same time to increase the sensitivity of the telescope-camera system.
Suggested apparatus for video capture can include modern astronomical video cameras, with USB connections to a computer, however they must be capable of recording video filmed in AVI file format. These videocameras must also have a good sensitivity at low light levels, such that there is sufficient contrast between the sky background, and the night (earthlit) side of the Moon. The camera sensitivity must be able to discern at least some recognizable features in Earthshine too, for the purpose of being able to detemine the map coordinates of the possible impact flashes. The time of each exposure should be set at shorter than 0.033 seconds (1/30 sec) if working at a frame rate of 30 fps; this is necessary because large numbers of lunar impacts have a flash durations of less than 1/10 sec, and so therefore it is important to record suspect flash impact flashes in at least two or three consecutive frames, and to be able to record both the flash luminosity peak as well as the decay of light curve as a function of time. Also it is of fundamental importance that the impact flash remains always fixed in the same position in all frames where it is visible, i.e. the flash must always light the same pixels of the sensor of the astronomical video camera used – so a tracking telescope is recommended. Not all candidate flashes seen are due to real impacts, the majority of flashes detected are in fact the result of cosmic rays air shower particles, that strike the camera, and appear and disappear in a very short time. However these cosmic rays usually create very bright points (and tracks) on the sensor and are visible in only one frame (Fig. 5 and 6). Also during the taking of video some terrestrial satellites can cross the lunar disk, and in this case they can appear as motion blurred streaks (Fig.7), or the slower ones appear as a moving bright spots across the lunar field. One way to check for satellites is to consult the web site of Heavens–Above or Calsky. NASA’s Marshall Space Flight Center developed some criteria for classifying the quality of candidate impact flash observations, for more information click here.
Captured image frames of candidate impact flashes, or any visual sightings, should be sent to the following e-mail address of the UAI Lunar Section luna@uai.it as JPEG images, or in PDF format for the visual observational reports. Please make sure that you always include the date and the time in UT for the suspected impact flash.
The project’s coordinator is Antonio Mercatali.
Orari per l'osservazione per il mese di Giugno 2015
Luna in fase calante, osservazione del lembo buio Est con inizio delle osservazioni dal sorgere della Luna e fino all’arrivo della luce dell’alba:
- 9 la Luna sorge alle ore 23:04 T.U. del giorno 8
- 10 “ alle ore 23:39 T.U. del giorno 9
- 11 “ alle ore 00:14 T.U.
- 12 “ alle ore 00.49 T.U.
- 13 “ alle ore 01:27 T.U.
- 14 “ alle ore 02:08 T.U.
- 15 “ alle ore 02:53 T.U.
Luna in fase crescente, osservazione del lembo buio Ovest con inizio delle osservazioni da quando fa buio e fino al tramonto della Luna:
- 17 la Luna tramonta alle ore 19:24 T.U.
- 18 “ alle ore 20:09 T.U.
- 19 “ alle ore 20.49 T.U.
- 20 “ alle ore 21.24 T.U.
- 21 “ alle ore 21.55 T.U.
- 22 “ alle ore 22:25 T.U.
- 23 “ alle ore 22.53 T.U.
- 24 “ alle ore 23:21 T.U.
