|
|||||
|
|
The Radio Observatory on the Lunar Surface for Solar studies |
|
| Authors: | T Joseph W Lazio RJ MacDowall Jack O Burns DL Jones KW Weiler L Demaio A Cohen N Paravastu Dalal E Polisensky K Stewart S Bale N Gopalswamy M Kaiser J Kasper |
| Institution: | 1. Remote Sensing Division, Naval Research Laboratory, 4555 Overlook Ave. SW, Washington, DC 20375-5351, USA;2. NASA Lunar Science Institute, NASA Ames Research Center, Moffett Field, CA 94089, USA;3. NASA/Goddard Space Flight Center, Code 695, 8800 Greenbelt Rd., Greenbelt, MD 20771, USA;4. Center for Astrophysics and Space Astronomy, Dept. of Astrophysical & Planetary Science, University of Colorado, Boulder, CO 80309, USA;5. M/S 138-308, Jet Propulsion Laboratory, 4800 Oak Grove Dr., Pasadena, CA 91109, USA;6. The Johns Hopkins University, Applied Physics Laboratory, 11100 Johns Hopkins Rd., Laurel, MD 20723, USA;g ASEE Engineering Fellow, 255 West 5th St, San Pedro, CA 90731, USA;h Physics Dept. and Space Sciences Laboratory, University of California, Berkeley, CA 94720-7300, USA;i Harvard-Smithsonian Center for Astrophysics, Perkins 138, MS 58, 60 Garden Street, Cambridge, MA 02138, USA |
| Abstract: | The Radio Observatory on the Lunar Surface for Solar studies (ROLSS) is a concept for a near-side low radio frequency imaging interferometric array designed to study particle acceleration at the Sun and in the inner heliosphere. The prime science mission is to image the radio emission generated by Type II and III solar radio burst processes with the aim of determining the sites at and mechanisms by which the radiating particles are accelerated. Specific questions to be addressed include the following: (1) Isolating the sites of electron acceleration responsible for Type II and III solar radio bursts during coronal mass ejections (CMEs); and (2) Determining if and the mechanism(s) by which multiple, successive CMEs produce unusually efficient particle acceleration and intense radio emission. Secondary science goals include constraining the density of the lunar ionosphere by searching for a low radio frequency cutoff to solar radio emission and constraining the low energy electron population in astrophysical sources. Key design requirements on ROLSS include the operational frequency and angular resolution. The electron densities in the solar corona and inner heliosphere are such that the relevant emission occurs at frequencies below 10 MHz. Second, resolving the potential sites of particle acceleration requires an instrument with an angular resolution of at least 2°, equivalent to a linear array size of approximately 1000 m. Operations would consist of data acquisition during the lunar day, with regular data downlinks. No operations would occur during lunar night. |
| Keywords: | Heliophysics Instrumentation: interferometers Moon Particle acceleration Radio astronomy |
| 本文献已被 ScienceDirect 等数据库收录！ | |