Solar imaging capabilities of the Brazilian decimetric array

Article Sidebar

PDF (Español (España))
Published: Jan 1, 2000
DOI: https://doi.org/10.22201/igeof.00167169p.2000.39.1.311
Keywords:
Sun, solar imaging, radio waves

Main Article Content

E. Lüdke
Uni. Federal de Santa Maria, CCNE - Dept. Física - LARIE, Santa María, RS, Brazil
https://orcid.org/0000-0002-3863-6069
H. S. Sawant
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
K. R. Subramanian
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil ; Indian Institute of Astrophysics, Koramangala, Bangalore, India
F. C. R. Fernandes
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
https://orcid.org/0000-0003-2922-3358
J. R. Cecatto
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
R. R. Rosa
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
https://orcid.org/0000-0002-2962-4322
J. H. A. Sobral
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
G. Swarup
Tata Institute of Fundamental Research, Pune Uni. Campus, Ganeshkhind, Pune, India
W. D. Gonzalez
Instituto Nacional de Pesquisas - INPE, São José dos Campos, SP, Brazil
C. E. Moron
Universidade Federal de São Carlos, UFSCar, Depto. Computação, São Carlos, SP, Brazil
M. L. Mucheroni
Universidade Federal de São Carlos, UFSCar, Depto. Computação, São Carlos, SP, Brazil

Abstract

In collaboration with the Universidad Federal de São Carlos (UFSC), the Instituto Nacional de Pesquisas, and the Universidad Federal de Santa María (UFSM) efforts are made to develop solar tomography using solar images obtained at various wavelengths from different observatories, in particular radio images, in order to predict occurrences of solar disturbances and related solar terrestrial and space weather effects. It is suggested that decimetric emission occurs near the solar regions where particles are accelerated or flare energy is released. However, no solar radioheliograph with sufficient time and spatial resolution at decimetric wavelengths has been built so far. In this paper, we describe the imaging capabilities of a T-shaped wideband solar heliograph operating at 1.2 - 1.7 GHz which is capable of obtaining solar disk images at 100 ms time resolution and angular resolution of ~4 arcminutes. With future hardware upgrades the final angular resolution will be 18 × 24 arcseconds which is comparable to X-ray images obtained with the YOHKOH satellite or radio images of the Nobeyama millimeter radioheliograph.

Article Details

How to Cite
Lüdke, E., Sawant, H. S., Subramanian, K. R., Fernandes, F. C. R., Cecatto, J. R., Rosa, R. R., … Mucheroni, M. L. (2000). Solar imaging capabilities of the Brazilian decimetric array. Geofisica Internacional, 39(1), 147–152. https://doi.org/10.22201/igeof.00167169p.2000.39.1.311
Issue
Vol. 39 No. 1 (2000): January 1, 2000
Section
Article
Creative Commons License

This work is licensed under a Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International License.

References

CLARK, B. G., 1980. Astron. Ap., 89, 377. DOI: https://doi.org/10.5594/J01613

CHOW, Y. L., 1972. IEEE Trans. on Anten. and Prop., AP-20 (1), 30. DOI: https://doi.org/10.1109/TAP.1972.1140131

CHRISTIANSEN, W. N. and J. A. HÖGBOM, 1987. Radiotelescopes, Cambridge Univ. Press, UK. CORNWELL, T. J. and P. N. WILKINSON, 1981. MNRAS, 196, 1067.

CORNWELL, T., 1995. Very Long Baseline Interferometry and the VLBI, ASP Conference Series Vol. 82, Ed. J. A. Zensus, P. J. Diamond, P. J. Napier. Gabriel A. H. et al.,1997, Solar Phys., 175, 207.

GONZALEZ, W. D., B. T. TSURATNI, P. J. McINTOSH and A. L. C. GONZALEZ, 1996. JGR. Lett., 23, 2577. DOI: https://doi.org/10.1029/96GL02393

HANAOKA, Y. et al., 1994, Proceedings of the Kofu Symposium “on New Look at the Sun with Emphasis on Advanced Observations of Coronal Dynamics and Flares”, Nobeyama Radio Observatory Report No. 360.

KOSUGI, T., K. MAKISHIMA, T. MURAKAMI, T. SAKAO, T. DOTANI, M. INDA, K. KAI, S. MASUDA, H. NAKAJIMA, Y. OGAWARA, M. SAWA and K. SHIBASAKI, 1991. Solar Phys., 136, 17 DOI: https://doi.org/10.1007/BF00151693

KOSOGI, T., 1994. Proceedings of the Kofu Symposium “on New Look at the Sun with Emphasis on Advanced Observations of Coronal Dynamics and Flares”, Nobeyama Radio Observatory Report No. 360.

NAKAJIMA, H. et al., 1984, Proc. IEEE, 82, 705. NAPIER, P. J., A. R. THOMPSON and R. D. EKERS, 1983. Proc. IEEE, 71, 1295. DOI: https://doi.org/10.1109/PROC.1983.12765

NARAYAN, R., R. NITYANANDA, 1986. Ann. Rev. Astron. Ap., 24, 127. DOI: https://doi.org/10.1146/annurev.aa.24.090186.001015

NISHIO, M., et al., 1994. Proceedings of the Kofu Symposium “on New Look at the Sun with Emphasison Advanced Observations of Coronal Dynamics and Flares”, Nobeyama Radio Observatory Report No. 360.

PEARSON, T. J. and A. C. S. READHEAD, 1984. Ann. Rev. Astron. Astrophys., 22, 97. DOI: https://doi.org/10.1146/annurev.aa.22.090184.000525

RAMESH, R., K. R. SUBRAMANIAN, M. S. SUNDARARAJAN and C. H. V. SASTY, 1998. Solar Phys., submitted.

ROSA, R. R., H. S. SAWANT, J. R. CECATTO, J. H. SAITO, C. E. MORON, M. L. MUCHERONI and N. FURUYA,1998(a), 32nd COSPAR Scientific Assembly proceedings, Nagoya, in press.

ROSA, R. R., et al., 1998(b), these proceedings.

SAWANT, H. S., K. R. SUBRAMANIAN, E. LÜDQUE, G. SWARUP, J. H. A. SOBRAL, F. C. R. FERNANDEZ, J. R. CECCATO and R. R. ROSA, 1998a, Proceedings of the VIII Simp. Brasileiro de Microondas e Optoeletrônica.

SAWANT, H. S., K. R. SUBRAMANIAN, E. LÜDQUE, J. H. SOBRAL, G. SWARUP, F. C. R. FERNANDEZ, R. R. ROSA, W. D. GONZALEZ and J. R. CECATTO, 1998b, Adv. Space Res., accepted.

SCHWAB, F., 1980, Proc. S.P.I.E., 231, 18. DOI: https://doi.org/10.1007/BF01588319

SRIVASTAVA, N., W. D. GONZALEZ and H. S. SAWANT, 1996, in: Proc. Chapman Conference on CMEs: causes and consequences, Bozeman, USA.

THOMPSON, A. R., J. M. MORAN and G. W. SWENSON, Interferometry and Synthesis in Radioastronomy, 1986, John Wiley & Sons, NY.