Faculty of Mathematics, Physics
and Informatics
Comenius University in Bratislava

AMOS Video Meteor Network

Development and establishment of AMOS all-sky video meteor cameras, as well as narrow-field video spectral cameras and creation of the Slovak Video Meteor Network led to the next target - the establishment of the worldwide meteor detection network. Even though there are multiple existing networks around the world, particularly in Europe, North America, Japan, Brazil, Australia, some areas of the globe remain without the coverage. This may particularly lead to a miss of short-living meteor shower with an activity of only hours. Continuous global coverage is also important for uninterrupted monitoring of major meteor showers and sporadic background. The latest still images from active cameras are available for preview. AMOS camera consists of fish-eye lens, image intensifier, digital video camera (frame rate 20/sec), operating computer with hard-drive, weatherproof enclosure, humidity and light sensors. The software used for transient detection is UFOCapture and for meteor orbit derivation UFOAnalyzer by SonotaCo. The software is being replaced by own improved proprietary software.


Current locations of AMOS cameras (red) : 4 cameras are in Slovakia (SVMN), 2 on Canary Islands (La Palma, Tenerife), 2 in Chile (San Pedro de Atacama, Paniri Cau - Chiu-Chiu). Planned locations (blue) in Hawaii, Namibia and Australia.



Therefore, we started to deploy AMOS cameras around the world. Initially, 4 cameras (since 2010) created a network in Slovakia (SVMN - Modra, Tesárske Mlyňany, Kysucké Nové Mesto, Važec).


Composite image of Perseid meteor shower on Aug 12/13, 2013 by AMOS.

 


Transient Luminous Event - Sprite - captured by AMOS in the upper right corner of the field.


In the next step, two cameras were installed in 2015 on Canary Islands - on Roque de los Muchachos observatory, La Palma and Teide, Tenerife. Both sites are on superb location, 2400 meters above sea level, with excellent seeing and low cloud coverage. The mutual distance is 143 km.

 


AMOS cameras with spectral cameras in Canary Islands.

Upper - Teide, Lower - Roque de los Muchachos.


Next giant leap was the installation of two cameras on the Southern Hemisphere, in Chile in 2016. Stations are installed at Paniri Cau Observatory, Chiu-Chiu and San Pedro de Atacama, 83 km apart. Chilean stations are more than 2400 m above sea level, also in excellent observing locations, with dark skies and low cloud coverage.



Installation of AMOS in Chile.



Milky way seen on a still image from AMOS in Chile, San Pedro.

 

 

Research

Meteor orbits can be derived when a meteor is observed at least from two stations at a distance where parallax allows measurement of the meteor trajectory in the atmosphere and derivation of the heliocentric orbit. We store our orbits in the Edmond database. Orbits of the meteors, coming from showers or the sporadic background, can be associated with the parent comets and asteroids. Also, the total flux of the meteoroid particles is particularly interesting for space agencies to assess the impact risk for their satellites. Meteor spectra and light curves are used for physical characterization of observed meteors, that can either reveal composition of Earth's atmosphere, molecules in the meteoroid particle and total strength of the matter of meteoroid.

 

Associated publications:

 1. Tóth J., Kornoš L., Vereš, P., Šilha, J., Kalmančok D., Zigo P.,    Világi J.: 2011, All-sky video orbits of Lyrids 2009, Publ. Astron.    Soc. Japan, 63, 311-314. 

2. Hajduková, M., Kornoš, L., Tóth, J. 2014, Frequency of hyperbolic    and interstellar meteoroids, Meteoritics and Planetary Science, 49,    63-68 

3. Rudawska, R., Zender, J., Jenniskens, P., Vaubaillon, J., Koten, P.,    Margonis, A., Tóth, J., McAuliffe, J., Koschny, D.: 2014,    Spectroscopic Observations of the 2011 Draconids Meteor Shower,    Earth, Moon, and Planets, 112, 1-4, 45-57 

4. Koten, P., Vaubaillon, J., Tóth, J., Margonis, A., Ďuriš, F.: 2014,    Three Peaks of 2011 Draconid Activity Including that Connected with    Pre-1900 Material, Earth, Moon, and Planets, 112, 1-4, 15-31 

5. Vaubaillon J., Koten P., Margonis A., Toth J. et al., 2015, The 2011    Draconids first European airborne meteor observation campaign,    Earth, Moon, and Planets, 114, 3-4, 137-157 

6. Rudawska R., Matlovič P., Tóth J., Kornoš L., Independent    identification of meteor showers in EDMOND database, Planetary and    Space Science, 118, 2015, 38-47

7. Kornoš L., Tóth J., Porubčan V., Klačka J., Nagy R., Rudawska R., On    the orbital evolution of the Lyrid meteoroid stream, Planetary and    Space Science, 118, 2015, 48-53 

8. Tóth J., Kornoš L.,  Zigo P., Gajdoš Š., Kalmančok D., Világi J.,    Šimon J., Vereš P., Šilha J., Buček M., Galád A., Rusňák P., Hrábek    P., Ďuriš F., Rudawska R., All-sky Meteor Orbit System AMOS and    preliminary analysis of three unusual meteor showers, Planetary and    Space Science, 118, 2015, 102-106 

9. Koten P., Vaubaillon J., Margonis A., Tóth J., Ďuriš F., McAulliffe    J., Oberst J., Double station observation of Draconid meteor    outburst from two moving aircraft, Planetary and Space Science, 118,    2015, 112-119

10. Rudawska R., Tóth J., Kalmančok D., Zigo P., Matlovič P., Meteor    spectra from AMOS video system, Planetary and Space Science, 123,    2016, 25-26

11. Hajduková, M., Jr., Koten, P., Kornos, L., Tóth, J., Meteoroid    orbits from video meteors. The case of the Geminid stream, Planetary    and Space Science, 143, 89-98

12. Matlovic, P., Tóth, J., Rudawska, R., Kornos, L, Spectra and    physical properties of Taurid meteoroids, Planetary and Space    Science, 143, 104-115

 

Future endeavors

We plan to expand our network around the world to increase thelongitudinal coverage of Earth. We are particularly interested in sitesthat do not have any meteor coverage and offer these minimumrequirements: dark skies, low cloud coverage, electricity and internetconnection, accessibility by road, and occasional light maintenance.

Grant support: APVV-0517-12, Slovak Research and Development Agency.

Principal Investigator: Dr. Juraj Tóth 

Host Institution: Comenius University in Bratislava, Slovakia