Institute of Solar-Terrestrial Physics

Transcription

1 Institute of Solar-Terrestrial Physics Observations of near-earth space objects at Sayan Observatory. Opportunities and future trends. V.Tergoev, Yu. Karavaev, E.Klunko, V.Goryashin, I.Korobtsev, M.Mishina, Т.Tsukker, M. Eselevich, P. Papushev Irkutsk, 2012 г.

2

3 Telescopes of Sayan Observatory ISTP RAS 0.6-meters telescope ZEISS-600 CCD: ST-6, FOV: 4,5' x 3,5', M lim =19 mag Tracking, photometry and op3cal surveys of near- Earth space objects 1,6-meters telescope AZT33-IR Cassegrainian focus(f/20) with optical reducer, CCD: S3C, FOV: 8,1' x 8,1', M lim =22 mag 0.5-meters upgraded telescope AZT-14 CCD: FLI PL4301E, FOV:1,3 x1,3, M lim =19 mag

4 Outline Observations of faint objects in GEO Detection of MEO debris. Some results Optical images of LEO objects in geophysical experiments Tracking of RadioAstron satellite (apogee=280000km) Prospective wide-field optical telescope Conclusions

5 Measurements of 250 small-size objects at Sayan Observatory in 2012 Longitude of Ascending Node vs. Inclina3on 80 Inclina3on (º) Longitude of Ascending Node (º) ARM < 1 ARM >=1

6 Photometric characteris3cs of the small- size objects with high area- to- mass ra3o (AMR) Photometric of objects with high AMR vary Average brightness: from 13 to 18 mag. Ø Amplitude of brightness from 0.5 to 2.5 mag. Ø Brightness periods : from several seconds to several minutes Ø Color- indexes (B- V): from 0.6 to 1.6 mag. AMR(m 2 /kg) B- V V- R Some objects show a constant brightness over observation session AMR=3.8 m2/kg AMR=31.8 m2/kg AMR=7.7 m2/kg (AMR=3.5 m2/kg) B-V =0.6 V-R= Phase Angle V B R (AMR=1.4 m2/kg) B-V = V-R= Phase angle V B R

7 Light curves of the small- size objects with high area- to- mass ra3o Objects with large period of brightness varia3ons AMR=2.1 m2/kg t_exp=3s Period=51.2s AMR=1.9 m2/kg t_exp-5s Period=60.8s AMR=2.7 m2/kg t_exp-5s Period=138.8 s AMR=21.4 m2/kg t_exp=1s Period=13s Objects with small period of brightness varia3ons AMR=1.2m2/kg t_exp=5s Period=? AMR=3.1 m2/kg t_exp=7s Period=? Bright object can be observed with short exposure Ime (~ 1s and less). This makes it possible to detect high- frequency brightness variaions. Observa@on of faint objects requires a large which can exceed the value of brightness varia@ons period. Therefore detec@on of short periods of such objects is a problem.

8 ObservaIons of the GLONASS satellites at the moment of orbital injecion

9 Unknown object in MEO MJD = ( ) T= a= м e= i= Ω= ω= n= day AZT-14 FOV=1.3 х1.3

10 Results of photometric observa3ons of several satellites of GLONASS constella3on Opera3onal spacecrazs 10 Glonass 727 ( 33466) UT=17:35:13 10 Glonass 744 ( 37867) UT=18:49: Glonass 794 ( 28113) UT=18:27: Non- opera3onal spacecrazs Glonass 795 ( 28114) UT=16:27: Period of brightness varia1ons 80s Period of brightness varia1ons 207s

11 LEO: observations of «Progress-M» onboard engine operations An opical observaions of cargo transport vehicle (CTV) «Progress- M» were performed during its onboard propulsion system operaions (September 2010 and April 2011, as a part of «Radar- Progress» acive space experiments). A typical CTV engine operaion Imes were seconds while distances from observatory were km (at the moments of engine start). The following phenomena were registered: A faint small «cloud» near CTV at the moments of engine start. A «jet» (rapidly changing in shape and brightness) which is the fuel paricles that are emiaed into space during a purging process aber engine shutdown. A shock occurs when fuel paricles collide with the environment material.

12

13 LEO: observations of «Progress-M» onboard engine operations Engine purging process between 6.7 and 9.3 seconds from engine start

14 High-altitude orbit Apogee~ km Perigee~70000 km RadioAstron s front view AZT-33 FOV=7.5'х7.5'

15 Wide-field telescope AZT-33ВМ Spectral range нм f 5600мм F/D 1:3,5 2ω 2,8 2y 277мм

16 Telescope D(м) 1 А(м 2 ) 2 Wide-field telescopes Ώ(град 2 ) 3 Θ(угл.сек) 4 SP 5 SP = AΩ θ 2 LINEAR Spacewatch UH 2.2-m/ PFCam Palomar/QUEST CFHT/Megacam S u b a r u / Suprimecam Pan-STARRS DMT/LSST АЗТ33 ВМ 1,6 2 6, ,3 1 Diameter ; 2 Area; 3 Spatial angle; 4 Image quality; 5 Survey performance(м 2 град 2 угл.сек -2 )

17 Conclusions Equipment of Sayan Observatory (SO) is successfully applied for measuring near-earth space objects in different types of orbits. High-precision trajectory and multi-color photometrical measurements performed at Sayan Observatory cover wide range of problems such as: determination of orbital parameters and photometrical characteristics of highapogee objects and obtaining images of LEO objects. Observations performed at SO make a considerable contribution to maintaining Russian catalog of high-apogee space objects. Observations confirmed the existence of a constantly growing fraction of small-sized space debris and possibility of its presence in MEO. Optical resources of SO are effectively used for controlling emergency situations, observing the processes of docking (undocking) of the ISS and CTV «Progress», controlling SPECTR-R satellite orbit (as a part of RadioAstron project). Solving current and prospective problems of guaranteed detection of dangerous space objects is ensured by manufacturing wide-field optical telescopes with high limit of detection. Scientific and technical start available at SO allows ISTP to complete building wide-field telescope AZT33VM on national experimental base by 2015.

18 Authors of the report express their gratitude and respect to their scientific head P.G. Papushev, who passed away January

19 Thank you very much!