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Evaluation of solar radio burst locator(SRBL) data from OVRO. 황보정은 1,2 , 봉수찬 2 , 조경석 2 , 문용재 2 , 이대영 1 , 박영득 2 , Dale E. Gary 3 , Brain L. Dougherty 4 1 Department of Astronomy and Space Science, Chungbuk National University. 2 Korea Astronomy and Space Science Institute

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evaluation of solar radio burst locator srbl data from ovro

Evaluation of solar radio burst locator(SRBL) data from OVRO

황보정은1,2, 봉수찬2, 조경석2, 문용재2, 이대영1, 박영득2, Dale E. Gary3 , Brain L. Dougherty4

1 Department of Astronomy and Space Science, Chungbuk National University.

2 Korea Astronomy and Space Science Institute

3 Physics Department, NJIT, University Heights

4 Solar Astronomy, Caltech, Pasadena

contents
contents

Ⅰ. Introduction

Ⅱ. Analysis of raw data (1998~2004)

Ⅲ. Analysis of flux error and location error(2000~2002)

Ⅳ. Summary

introduction background
Ⅰ. Introductionbackground
  • SRBL (Solar Radio Burst Locator) is a

spectrometer that can observe solar

microwave burst over wide band(0.1-18 GHz)

as well as detect the burst location without

interferometry or mechanical scanning

  • KASI plans to make the K-SRBL system

to locate solar microwave bursts and

solar microwave spectra

  • We need to analyze the data from the

solar radio burst locator in Owens Valley

Radio Observatory

NJIT have been running SRBL of OVRO

relative intensity versus frequency for different burst locations
Relative intensity versus frequency for different burst locations.

SRBL’s log-spiral feed

  • At antenna-center
  • half way to West side
  • 3) at West limb
  • 4) at East limb.
  • Such modulations appear throughout
  • burst and quiet-sun spectra, forming
  • the basis of SRBL’s location capability.
slide6

Ⅲ. Analysis of flux error and location error(2000~2002)

1) Comparison the SRBL flux with RSTN’s

  • We chose 55 SRBL events whose maximum-flux frequency is consistent with the RSTN frequency within 10%.
  • There is a good correlation (r=0.9) between these two fluxes.
  • This fact implies that the flux measurement by the SRBL is consistent with that by the RSTN, demonstrating the proper measurement of solar microwave burst flux by SRBL system.
location error vs x ray intensity
Location Error VS X-ray Intensity
  • This is the relationship between location error and X-ray peak flux for the 25 events. The location error is much more widely scattered for multiple source and weak intensity events than single source and strong intensity events.
  • The multiple source events usually have larger location errors than the single source events.
m e time vs burst start time and peak time
M-E time VS Burst Start Time and Peak Time
  • The M-E (minimum error) time that is defined as the time when the location error is minimum.
  • We present the relationship among the M-E time, burst start time, and burst peak time. There is a strong tendency that the M-E time was mostly located just after the starting time.
pointing error
Pointing error
  • The pointing error is defined as the difference between solar center and antenna center, which is estimated from quiet sun spectrum taken just before the burst.
  • The anti-correlation becomes more evident (r=-0.9) when we only consider 6 single source events related with strong (X-class) flares.
summary
Ⅴ. summary
  • There is a relatively good correlation (r=0.9) between SRBL flux and RSTN flux. This result indicates that the SRBL flux is consistent with the RSTN flux
  • The multiple source events usually have larger location errors than those of the single source events. It is also noted that the mean location error near the flaring time for single source events is found to be about 4.7 arcminutes.
  • The M-E time (minimum error) to estimate the burst location, when the error is minimum, is found to be just after the burst starting time, mostly within 10 seconds.
  • There is an anti-correlation (r=-0.4) between the pointing error and the location error. Such an anti-correlation becomes more evident (r=-0.9) for 6 strong single source events associated with X-class flares.