IPS at Ooty Observatory Report Ooty Radio Ooty
IPS at Ooty – Observatory Report
Ooty Radio Ooty Telescope Radio Telescope (ORT) • • • Equatorially mounted 530 m (N-S) x 30 m (E-W) East-west tracking of ~9. 5 hours North-South beam steering (about ± 60 deg. declination) High sensitivity, S/N ~ 25 (1 s integration, BW 4 MHz) http: //rac. ncra. tifr. res. in
Ooty Radio Telescope is operated by National Centre for Radio Astrophysics, Tata Institute of Fundamental Research. • Routine IPS observations are being made at Ooty and these measurements extremely useful for • Studies of solar wind in the inner heliosphere • Understanding propagation of coronal mass ejections (CMEs); Ooty IPS studies provide a complete coverage to image CME structures all the way from the Sun to the orbit of the Earth. Ooty Radio Telescope has been upgraded. The following slides shows typical IPS source coverage before and after upgrade,
Typical source distribution before the upgrade
Typical g-map before the upgrade
Typical source distribution after the upgrade
G-map for the upgrade Ooty Telescope
Radial Dependence of Density Turbulence Monitoring of IPS at Ooty on several compact radio sources, over several years, has provided m-p curves, which have been useful to estimate the radial dependence of density turbulence in the distance range of ~40 – 225 solar radii (i. e. , weak-scattering regime at 327 MHz).
‘Turbulence – Distance’ Dependence Sample m-p curves for 2 compact radio sources δNe (R) ~ R-β
Radial Dependence of Solar Wind Turbulence (β) ~ (R) ~ R-2β Solar wind seems to expand steeper than spherically symmetric expansion
Radial Dependence of Density Turbulence At heliocentric distance R > 40 solar radii, β does not show significant variation with solar cycle
Shock Formation Height CALLISTO installed at Ooty (RAC-NCRA) provides records solar radio bursts. The solar radio spectrum combined with the SDO images has been useful to understand the formation height of type-II emission (i. e. , the shock formation height)
Ooty CALLISTO
Thank You
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