Comparison of Orbital and Physical Characteristics of Bright and Faint GEO Objects
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1 Russian Academy of Sciences Keldysh Institute of Applied Mathematics Comparison of Orbital and Physical Characteristics of Bright and Faint GEO Objects V.Agapov 1, I.Molotov 1, Z.Khutorovsky 2 1 Keldysh Institute of Applied Mathematics, Russian Academy of Sciences, 2 Interstate Corporation Vympel 2010 AMOS Conference Wailea, Maui, September 2010
2 Research Goals Understanding deterministic GEO object population distribution by various parameters Verification of applicability of diffuse sphere model usage for statistical modeling of GEO objects brightness distribution Understanding approaches which can be used for brightness estimation in sensor tasking for survey and track modes Checking consistency in observed brightness patterns for objects of the same design 2
3 GEO region definition (KIAM database) Inclination range 0 30 Eccentricity 0.2 Period range min (corresponds to mean motion range approx rev/day) 3
4 I S O N International Scientific Optical Network 4
5 GEO Population Knowledge (KIAM database, Sep 1, 2010) Total 1530 objects in GEO region with orbits maintained routinely, including Spacecraft under control, 502 non-functional Upper stages and AKMs 256 Fragments and objects of undetermined type 365 5
6 Observed Individual GEO Objects Number (by night, Jan Jun 2010) 6
7 Distribution of 1530 GEO objects by period and inclination 7
8 Distribution of 1530 GEO objects by RAAN and inclination 8
9 Observability of GEO Objects for ISON telescopes GEO objects having magnitude around 16.2 m or brighter are observing routinely by ISON survey telescopes of cm class GEO objects having magnitude around between 16.2 m and 18 m are detecting and tracking by ISON telescopes of cm class GEO objects having magnitude fainter than 18 m are detecting and tracking by ISON telescopes of 1 m class and larger 9
10 Bright and Faint Objects Bright magnitude 16 m 16.2 m or brighter Faint magnitude fainter than 16.2 m no filters phase angle range 0-20 more than 80% of measured brightness values fall into one of two categories 10
11 Estimation of brightness of a diffuse sphere at GEO distance Potential limit of detection for ISON survey cm telescopes in a survey mode with sec integration time Potential limit of detection for ISON survey and tracking cm telescopes 11
12 Distribution of 1530 bright and faint GEO objects by RAAN and inclination 12
13 Characteristics of Objects Derived from Processing of Optical Orbital parameters Measurements AMR (mean, variations) Brightness pattern (mean, variations, proximity to diffuse sphere model) Further correlation of AMR and brightness with an object of specific shape and mass can be studied mainly for bright known objects 13
14 Bright Objects Spacecraft (designed on the base of more than 150 primary buses and their modifications), rocket bodies and AKMs (of more than 20 different types and modifications), large operational fragments and some of fragments of unknown type compose the group Mainly very low AMR (<0.1 sq.m/kg) objects Various brightness variation patterns Brightness in many cases can not be modeled using diffuse sphere model 14
15 INTELSAT IV HS-312 bus 7 objects, 6535 measurements, 24 telescopes Brightness corrected for range only (40000 km) 15
16 INTELSAT IV No phase correction Diffuse sphere phase function applied Do not looks like a diffuse sphere 16
17 TITAN IV CENTAUR R/B L=8.94 m D=4.51 m 10 objects, measurements, 31 telescopes Brightness corrected for range only (40000 km) 17
18 TITAN IV CENTAUR R/B No phase correction Diffuse sphere phase function applied Looks like a diffuse sphere in a certain range of phase angles 18
19 Spacecraft of GORIZONT Type (Not Operational) 26 objects, measurements, 26 telescopes Brightness corrected for range only (40000 km) 19
20 GORIZONT SPACECRAFT (Not Operational) No phase correction Diffuse sphere phase function applied Looks like a diffuse sphere in a wide range of phase angles!!! 20
21 AMR for Bright Objects For the absolute majority of bright objects AMR do not exceed 0.1 sq.m/kg There are a few unique exceptions. The most interesting are AMR=0.6 sq.m/kg AMR=1.7 sq.m/kg AMR=21 sq.m/kg 21
22 Object AMR=0.6 sq.m/kg 4946 measurements, 18 telescopes Brightness corrected for range only (40000 km) Brightness variations up to 7.5 mag!!! 22
23 Object AMR=0.6 sq.m/kg No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness estimation is not applicable 23
24 Object AMR=1.7 sq.m/kg 2039 measurements, 14 telescopes Brightness corrected for range only (40000 km) Brightness variations up to 9 magnitudes with observed 9 th -10 th mag!!! 24
25 Object AMR=1.7 sq.m/kg No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness estimation is not applicable 25
26 Object AMR=21 sq.m/kg Magnitude vs. Phase angle Phase angle vs. Range 8337 measurements, 22 telescopes Brightness corrected for range only (40000 km) Very bright and very high AMR 26
27 Object AMR=21 sq.m/kg No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness estimation is applicable only in a narrow range of phase angles 27
28 Faint Objects Only fragments and objects of undetermined type compose the group Mainly high AMR (>0.9 sq.m/kg) objects Various brightness variation patterns Brightness in most cases can not be modeled using diffuse sphere model 28
29 Number of Obj. Brightness distribution for GEO fragments and objects of undetermined type Magnitude Distribution of average brightness for 434 fragments 29
30 Number of Obj. AMR distribution for GEO fragments and objects of undetermined type Area-To-Mass Ratio, m 2 /kg Distribution of average AMR value for 211 fragments 30
31 Faint Objects AMR<0.9 sq.m/kg, 16 m < Mag < 17.5 m 80 objects, measurements, 23 telescopes Brightness corrected for range only (40000 km) 31
32 Faint Objects AMR<0.9 sq.m/kg, 16 m < Mag < 17.5 m No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness seems applicable in a certain range of phase angles 32
33 Faint Objects AMR>=0.9 sq.m/kg, 16 m < Mag < 17.5 m 112 objects, measurements, 32 telescopes Brightness corrected for range only (40000 km) 33
34 Faint Objects AMR>=0.9 sq.m/kg, 16 m < Mag < 17.5 m No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness seems applicable in a certain range of phase angles 34
35 Faintest Objects AMR<0.9 sq.m/kg, Magnitude > 17.5 m 21 object, measurements, 17 telescopes Brightness corrected for range only (40000 km) 35
36 Faintest Objects AMR<0.9 sq.m/kg, Magnitude > 17.5 m No phase correction Diffuse sphere phase function applied Model of diffuse sphere for brightness seems applicable in a wide range of phase angles 36
37 Faintest Objects AMR>=0.9 sq.m/kg, Magnitude > 17.5 m 49 objects, measurements, 16 telescopes Brightness corrected for range only (40000 km) 37
38 Faintest Objects AMR>=0.9 sq.m/kg, Magnitude > 17.5 m No phase correction Diffuse sphere phase function applied Difference with lower AMR faintest objects is minimal 38
39 Conclusions ISON network collects on a routine basis astrometric and brightness measurements for more than 1500 objects in GEO region Accumulated measurements can be used for statistical characterization of GEO population It is revealed that the model of diffuse sphere reflection is not applicable in many cases both for bright and faint GEO objects Distribution of measured brightness values within defined phase angle subranges is very close to the normal (Gaussian) for majority of bright and faint GEO objects There are unique objects (presumably fragments) having unusual properties in terms of AMR and brightness. They should be studied individually 39
40 Acknowledgements We are very thankful to all ISON participants whose routine work permits to collect large amount of information for GEO population study Special thanks to the AIUB team working in collaboration with us for more than 5 years already and providing a lot of valuable data on the newly discovered faint debris in GEO 40
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