Low Frequency Radio Astronomy from Above the Ionosphere
Explore the source record for details and available documents.
Engineering topics
Publications and source records attributed to Jones, D..
Explore the source record for details and available documents.
During the latter half of the 1980's three concepts for low frequency arrays on the Moon were independently studied for NASA, leading to two workshops in 1990. The main technical challenges were those of deploying the array on the Moon, and of correlating the data on the Moon or returning all the raw data to Earth.
Explore the source record for details and available documents.
Explore the source record for details and available documents.
The VLBA's high angular resolution at 22 and 43 GHz allows the nuclei of nearby radio galaxies to be imaged with very high linear resolution. This is the scale on which absorption by the dense ionized inner regions of nuclear accretion disk should be detected.
We have imaged the nucleus of the nearby radio galaxy NGC 4261 (3C270) with the VLBA at 1.6, 8.4, 22, and 43 GHz. At 8.4 GHz our image reveals a narrow gap in emission just east of the core, which we interpret as absorption by an inner accretion disk seen nearly edge-on.
The structure of AGN accretion disks on sub-parsec scales can be probed through free-free absorption of synchrotron emission from the base of symmetric radio jets.
A radio interferometer array in space providing high dynamic range images with unprecedented angular resolution over the broad frequency range from 0.030 - 30 MHz will open new vistas in solar, terrestial, galactic, and extragalactic astrophysics.
Explore the source record for details and available documents.
The Einstein ring gravitational lens PKS 1830-211 consistents of two bright, milliarcsecond-scale radio components separated by 1 arcsec and connected by a fainter ring of radio emission (Rao and Subrahmanyan 1988; Jauncey et al. 1991).
The double-lobed radio galaxy NGC 4261 (3C270) contains a pair of highly symmetric kpc-scale jets, as well as a two-sided morphology on parsec scales.
A study of several Harris current sheet type Euler potential models of Jupiters magnetosphere is presented.
A planet orbiting a rado-emitting star can be indirectly detected by high-precision Very Long Baseline Interferometry (VLBI) astrometry through the reflex orbit of the star.
The radio-luminous supernova SN 1993J in M81 offers an unprecedented opportunity to study with high linear resolution the details of the growth of a supernova radio structure by means of the VLBI technique.
The strong radio source PKS 1830-211 consists of two compact components located on opposite sides of a fainter ring of radio emission 1 arcsecond in diameter.
We present a comparison of VLBI and Hipparcos astrometric parameters of several optically bright radio-emitting stars.