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Moscow
2006
Astro Space Center
P.N. Lebedev Physical
Institute
DCR-1000 - cross 1000х1000 m,
width 40 m, range 30-120 MHz.
BSA – array of 16384 dipoles,187х384 m,
16 separate beams, range 110±1 MHz.
RT-64, Kalyazin
RT-22, Pushchino
Solar wind turbulence spectrum. Observations of radio signals
scintillations of distant spacecrafts. In acceleration region was found
flicker noise spectrum, in more distant quite region – cascade
Kolmogorov spectrum (Chashey I.V. at collaboration).
Interstellar plasma turbulence spectrum by observation scintillation
of pulsars radio emission in scales of few 103 km to 1013 km.
Spectrum is very near to Kolmogorov with index 11/3 (Chashey I.V.
at al.).
Radio emission of two short period X-ray pulsars was found in the
centers of supernova remnants.
•
PSR J0205+6449 in the 3С58, very young
neutron or quark star, age about 850 years.
• BSA observations at 111 MHz
• a) accumulation of five periods interval by
observations of 1145 pulses.
• b) accumulated one period (65.68 ms) by
observations of 5725 pulses.
• Radio flux 40 mJy, magnetic field 7*1012 G,
distance 6.4 kps.
Malofeyev V.M., Malov O.I., Malov I.F., Teplykh D.A., Glushak A.P.
Super giant pulse of Crab nebula pulsar: flux 7·106 Jy at 2.2 GHz, TB = 1040 K.
E and H of the electromagnetic wave larger the pulsar magnetic field H~1012 G.
RT-64, Kalyazin (Popov M.V., Soglasnov V.A. et al.).
8 МЯн
Радио
Оптик
а
Рентген
6
4
2
0
0
2
4
Period of neutron star rotation is 33 ms.
6
8
мкс
Flare of maser OH (1665 MHz) emission in the star
formation region W75N, distance 2 kps
(Slysh V.I. et al., 2005).
Калязин
Калязин
Нансэ
VLBA
VLBA
VLBA
VLBA
More 25 years of H2O space masers monitoring at 22 GHz
in PRAO. It’s the most long set observations. 125 sources
are in the modern list for observation once in the month.
Here two type sources: super compact (~1au) gaze clouds
in star formation regions and envelopes of variable late
spectra classes stars.
In star formation regions was found periodicity of masers
variations (few years periods). This sources have usually
three spectral components and probably correspondent to
proto planet disks formed around proto star.
It was found that variability of masers in stars envelopes
strong correlate with IR and optic variation of the star at
definite delay. It’s confirm a shock model, which
propagates from the star across envelope.
Here demonstrated a maser and optics observations in
2000-2004 of variable star в 2000-2004 гг и оптического
блеска переменной звезды V391 Cyg. Delay is 100-150
days.
(RT-22, LPI and SAI collaboration, Samodurov V.A. et al.).
New method of Universe parameters
determination by SMB analysis.
Project GLESP (Gauss-LEgendre Sky
Pixelization) for PLANCK
mission
(2007). As expected this method will
be used for determination of the dark
matter and dark energy, neutrino
mass, Hubble constant, spectrum of
density perturbation, spectrum of
primordial gravity waves, parameters
of secondary ionization and others
with accuracy 1%.
A.G. Doroshkevich, P.D. Naselsky, O.V. Verhodanov, D.I. Novikov,
V.I. Turchaninov, I.D. Novikov, P.R. Christensen, L.-Y. Chiang,
Inter . J. Modern Physics D (2005)
Inflation stage Universe parameters
determination.
New model (Lambda-inflation)
permit by observation data on
density galactic clusters and CMB
anisotropy to find limitations on
model parameters and amplitudes
of primordial gravitational waves
(vertical axis) and spectral index
density perturbations (horizontal
axis).
V.N.Lukash, E.V.Mikheeva, V.Muller, A.M.Malinovsky, MNRAS (2000)
V.N.Lukash, E.V.Mikheeva, Inter. J. of Modern Physics A (2000)
Е.В.Михеева, В.Н.Лукаш, Астроном. Журнал (2004); В.Н.Лукаш, УФН (2006)
LogN-logS distribution of gammabursts
(most deep set)
The circles – previous date.
Crosses – a new distribution of
3906 all found bursts in BATSE
archive data by new method..
B. Stern, Ya. Tikhomirova, D. Kompaneets, R. Svensson, J. Poutanen, ApJ (2001)
Kalyazin Radio
Observatory.
RT-64 beamwidths
are ~11' at 1.4 GHz
and ~7' at 2.3 GHz.
The expected events
should be near the
limb of the Moon,
so the pointing was
at 14' apart from
the center of the Moon
(Dagkesamanskiy R.D. et
al.).
Position of the
antenna beams on the
Moon
ARENA-2005
Detection of Ultrahigh-Energy Cosmic Rays and neutrinos
by Radio Method
LUNAR
ORBITAL
RADIO
DETECTOR
LPI, Lavochkin Association,
MSU, IAS, JINR, ISP (Sweden)
expected launch
2009
V.Tsarev, e-mail
[email protected]
Radio Galaxy M87 (red shift 0.0044)
The internal jet is strong vary with time but most compact
unresolved detail is seeing always. It’s super massive black
hole of 3 billion solar mass, diameter smaller 10 light days,
flux 0.2 Jy. (VLBA at 15 GHz observations for RadioAstron
mission).
Kovalev et al. (2005)
April
June11,
10,
18,2005
2005
2005
April
Jansky
Symposium,
NRAO
Blazar
Variability
Workshop
II
Arecibo Observatory
Library
Colloquium
Compactness (ratio of unresolved component flux to total flux) histogram: the
most variable sources are more compact. 250 objects of VLBA observations
at 15 GHz for RadioAstron mission program. (Kovalev Yu.Yu. et al., AJ, 130,
2473-2505 2005)
North hemisphere sources for RadioAstron program.
Red points – sources with normal specters, green points the sources
with inverted specters.
(Larionov M.G. et al. 2005). (Ларионов М.Г. и др., 2005 г ).
RADIO INTERFEROMETER MUCH LARGER
THE EARTH
“SPECTR-R” (Mission “RadioAstron”)
Main scientific tasks of the mission –
syntheses of high-precision images of various Universe objects, its
coordinates measurements and search their variability with the time.
A fringe width of the system is
up to 7 micro arc seconds.
Main characteristics of the space radio telescope
Spectral band:

wavelength (cm) 92;
18;
6.2;
1.19-1.63

frequency (GHz) - 0.327; 1.66; 4.83;
18-26
Main organizations:
on scientific complex - Astro Space Center of Lebedev Physical Institute of
Russian Academy of Science;
of spacecraft - Lavochkin Research Production Association of Russian Space
Agency.
Planned launch date of the mission is 2007.
The orbit of the mission :
apogee 310 000 - 370 000 km
perigee 10 000 - 70 000 km
declination 51.6 °
period variation 7 - 10 days
Guarantied time of activity 5 years
Scientific payload mass 2100 kg
Pointing accuracy of radio telescope - 35"
OBJECTS OF EXPLORATION BY RADIOASTRON MISSION
1.
GALAKTIC NUKLEI (SYNCHROTRON EMISSION, COSMIC RAYS,
MEGAMASERS, BLACK HOLES, WORMHOLES, NEW PHYSICS).
2.
COSMOLOGY, DARK MATTER AND DARK ENERGY, TIME-SPACE
METRIC BY OBSERVATIONS OBJECTS AND GRAVITATION LENSES
AT DIFFERENT REDSHIFTS.
3.
STAR AND PLANETARY SYSTEM FORMATION REGIONS (MASERS).
4.
STELLAR MASS BLACK HOLES AND NEUTRON (QUARC?) STARS.
5.
INTERSTELLAR AND INTERPLANETARY PLASMA.
6.
HIGH ACCURACY COORDINATE SYSTEM AND FUNDAMENTAL
ASTROMETRY.
7.
HIGH ACCURACY BALLISTIC AND PRECISION EARTH GRAVITY
FIELD.

The main expectable goals of Radioastron mission
Super massive black holes in galactic nuclei: behavior of the matter near the events
horizon, the structure and value of magnetic field near internal accretion disc and
near black hole poles, mechanism of the relativistic particle acceleration (protons
or/and electron/positron pairs, direct detection of cosmic ray acceleration sources,
Blanford-Znajek or/and electric field in vacuum acceleration), evolution of this
parameters in cosmological time scale and the role of normal and dark matter),
 super luminal motion and expansion of radio sources at different redshifts, dark
matter distribution from the lensing superluminal sources,
 cosmological proper motions of extragalactic radio sources,
 black holes and neutron stars in our galaxy (a study of the energy production
mechanism, determination of distance and proper motion, Galaxies gravity
potential from pulsar proper motion observations, measurements of relativistic
binary system orbits),
 interstellar plasma in Galaxy (scintillation of fringe visibility and refraction
phenomena by pulsar observations),
 young stars and planets (a study of the structure and dynamics of the star-birth
regions in galaxies by their megamaser emission, a study of young stars and
protostars with protoplanetary rings in our galaxy by their maser emission),
 3D Earth gravity field and fundamental astrometry with high accuracy.
More than 6000 objects in total are accessible to Radioxplorations with
highest angular resolution.
Megamaser in the galaxy NGC4258
(6.4 million pc)
РТ-70 миллиметрового
диапазона на плато Суффа.
Миллиметровый РТ-70.
MILLIMETRON.
12 m cryogenic mirror.
λ = 0,01-20 mm.
Bolometric sensitivity
5*10-9 Jy (σ)
(λ=0.3 mm, 1 hour int.).
Space-ALMA VLBI
sensitivity 10-4 Jy (σ)
(λ=0.5 mm, 300 s int.),
fringe size up to
nanoarcseconds.
Ground-space Interferometer
Millimetron
ALMA
Suffa
(Uzbekistan)
Space-based Interferometry