Joseph Fainberg | Johns Hopkins University (original) (raw)
Papers by Joseph Fainberg
Twelve type 2 solar radio events were observed in the 2 MHz to 30 kHz frequency range by the radi... more Twelve type 2 solar radio events were observed in the 2 MHz to 30 kHz frequency range by the radio astronomy experiment on the ISEE-3 satellite over the period from September 1978 to December 1979. These data provide the most comprehensive sample of type 2 radio bursts observed at kilometer wavelengths. Dynamic spectra of a number of events are presented. Where possible, the 12 events were associated with an initiating flare, ground based radio data, the passage of a shock at the spacecraft, and the sudden commencement of a geomagnetic storm. The general characteristics of kilometric type 2 bursts are discussed.
Benson et al. (2015, this volume) selected 10 large magnetic storms, with associated Dst minimum ... more Benson et al. (2015, this volume) selected 10 large magnetic storms, with associated Dst minimum values less than or equal to -100 nT, for which high-latitude topside ionospheric electron density profiles are available from topside-sounder satellites. For these 10 storms, we performed a superposition of Dst and interplanetary parameters B, v, N(sub p) and T(sub p). We have found that two interplanetary parameters, namely B and v, are sufficient to reproduce Dst with correlation coefficient cc approximately 0.96 provided that the interplanetary parameter times are taken 0.15 days earlier than the associated Dst times. Thus we have found which part of the solar wind is responsible for each phase of the magnetic storm. This result is also verified for individual storms as well. The total duration of SRS (storm related structure in the solar wind) is 4 - 5 days which is the same as the associated Dst interval of the magnetic storm.
Long duration storms of type III radio bursts were discovered in the hectometer wavelength range ... more Long duration storms of type III radio bursts were discovered in the hectometer wavelength range during the last solar cycle, utilizing the RAE-1 satellite observations. The major results are discussed including the investigation of the average exciter speed, the density of the regions (streamers) in which they are produced, the degree of inhomogeneity of the medium and the solar wind speed. During the present solar maximum, the ISEE-3 radio experiment has provided a unique means of monitoring radio emissions in the interplanetary medium from about 10 to 215 solar radii, with an almost continuous time coverage. The authors review preliminary results of this analysis, including the correlation with the solar activity and with type I and type III storms.
Radio Physics of the Sun, 1980
We present simultaneous energetic electron and solar radio obser vations from the ISEE-3 spacecra... more We present simultaneous energetic electron and solar radio obser vations from the ISEE-3 spacecraft of several solar type III radio bursts, ^he UC Berkeley energetic particle experiment measures from 2 to ^ 10 keV with good energy and pitch angle resolution while the Meudon/GSFC radio experiment tracks type III radio bursts at 24 fre quencies in the range 30 kHz-2 MHz. Two types of electron events are observed by the particle experi ment: (1) the "normal" type of 20 to > 100 keV flare associated elec tron events reported previously, and (2) events where only electrons in the 2-10 keV range are observed. These low energy, 2-10 keV, elec tron events appear not to be associated with flares or high frequency (> 10 MHz) radio emission as reported in the Solar Geophysical Data bulletins, but rather they appear to be associated with individual type III bursts from low frequency type III storms. Both types of electron event are closely correlated to the very low frequency type III emission produced in situ at 1 A.U. The radio experiment is able to identify the direction of arrival of the radio emission through a combination of a dipole antenna spinning in the ecliptic plane plus z-axis antennas for out-of-the-ecliptic direction. The frequency of the radio emission pro duced in situ around the spacecraft can be identified by its omnidirec tional nature. We have compared the temporal behavior of the in situ radio intensity and the electron intensity. In every case good agree ment was found between the onset times for the in situ radio and elec tron events. For the single event where solar wind plasma density measurements were available the frequency of the radio emission is con sistent with the emission being generated at the second harmonic and not at the fundamental of the plasma frequency. We have made preliminary computations of the electron velocity distribution function parallel to the magnetic field, f(vjj), for several^events. In the > 20 keV events no strong positive slope ^ > 0 is observed, rather f(vj|) has a plateau-like shape, even dv |(311
Astronomy and Astrophysics, 1985
An analysis is presented of the system response of a satellite receiver-antenna system to locate ... more An analysis is presented of the system response of a satellite receiver-antenna system to locate a radio source when the satellite is tilted on its axis. The satellite is spin stabilized but experiences a tilt due to either a mechanical misalignment or a shift in the electrical axis caused by parasitic currents in other spacecraft structures. The shorter the antenna, the more significant the effects. Numerical techniques are developed for obtaining the Stokes parameters and the angular parameters of a uniform conical source sensed by a linear antenna in order to derive the average power response of a synthesized dipole to a point on a distributed polarized source. Relative gains are calculated along the antenna at different angles to the source. The techniques are applied to sample ISEE-3 satellite data for Type III solar radio bursts which were sensed by an axial and an equatorial antenna. The two antennas permit localization of the source and quantification of the polarization and...
General Assembly and Scientific Symposium, 2011
Geophysical Research Letters, 1996
We analyze 2f p radio emission observed during a perigee pass in August 1995 when the WIND spacec... more We analyze 2f p radio emission observed during a perigee pass in August 1995 when the WIND spacecraft was between 47 and 72 R E from Earth and upstream of the electron foreshock. The WAVES experiment on WIND measures the direction of arrival and complete polarization state of the 2f p radiation. We found no evidence for significant linear or circular polarization. For one period when we were able to utilize the direction finding capability to determine the actual 2f p source location, using an interplanetary shock as a diagnostic, the radio emitting region was confirmed to lie within the electron foreshock near the contact point. We indicate how such remotely observed 2f p emissions can be used to monitor the response of the electron foreshock to instantaneous changes in the interplanetary magnetic field.
Geophysical Research Letters, 1998
We discuss the thermal evolution of the spurion and messenger fields of ordinary gauge mediation ... more We discuss the thermal evolution of the spurion and messenger fields of ordinary gauge mediation models taking into account the Standard Model degrees of freedom. It is shown that for thermalized messengers the metastable susy breaking vacuum becomes thermally selected provided that the susy breaking sector is sufficiently weakly coupled to messengers or to any other observable field.
Geophysical Research Letters, 2001
![Research paper thumbnail of Interplanetary baseline observations of type 3 solar radio bursts. [by Helios satellites]](https://attachments.academia-assets.com/78430765/thumbnails/1.jpg)
](The first simultaneous observations of type III radio bursts using spacecraft separated by severa... more The first simultaneous observations of type III radio bursts using spacecraft separated by several tenths of an AU have been made using the solar orbiters HELIOS-A and-B. The burst beginning at 1922 UT on March 28, 1976, has been located from the intersection of the source directions measured at each spacecraft, and from the burst arrival time differences. Wide baseline observations give the radial distance of the source at each observing frequency. Consequently, coronal electron densities and exciter velocity were determined directly, without the need to assume a density model as has been done with single spacecraft observations. The separation of HELIOS-A and-B has also provided the first measurements of burst directivity at low frequencies. For the March 28 burst the intensity observed from near the source longitude (HELIOS-B) was significantly greater than from 60 0 W of the source (HELIOS-A).
Two examples of type 2 radio emissions associated with the propagation of earth-directed coronal ... more Two examples of type 2 radio emissions associated with the propagation of earth-directed coronal mass ejections (CMEs) through the interplanetary medium are illustrated and compared. The two type 2 radio events were observed by WIND/WAVES in January and May of 1997 and exhibit very different radio characteristics. The analyses presented here use the novel approach of presenting the radio data as a function of the inverse of the frequency and time, which facilitates remote radio tracking of the CME through the interplanetary medium. It is demonstrated unequivocally that for the May 1997 event, the radio emissions were generated at the fundamental, and harmonic of the plasma frequency in the ambient plasma upstream of the CME-driven shock. For the January 1997 event, evidence is presented that some of the radio emissions were generated while the CME-driven shock passed through a corotating interaction region (CIR). This is the first time that type 2 radio emissions were shown to origi...
[
... radio experiment at ISEE 3, about one hour earlier in accordance with the transit time of ...... more ... radio experiment at ISEE 3, about one hour earlier in accordance with the transit time of ... However, these positions may have systematic errors if significant linear polarization is present in the observed ... Intensity variations of 20 db and apparent motions of 40 R E can occur with ...
The Ulysses URAP experiment has provided the first measurements of remote and in-situ wave phenom... more The Ulysses URAP experiment has provided the first measurements of remote and in-situ wave phenomena from high southern latitudes. Remote sensing of type 3 solar radio bursts constitute an important component of the Ulysses observations. Type 3 radio emissions, which have never before been viewed from outside the ecplitic plane, have been observed by Ulysses to its maximum southern latitude (approximately 80 deg S), although their frequency of occurrence has generally diminished due to the declining phase of the solar cycle. In addition, the Ulysses radio receiver measures both the direction of arrival and the complete polarization state of incident radiation. These physical parameters provide information on the origin and nature of the radio emission. Preliminary analyses have indicated that kilometric type 3 radiation is often approximately 10-20% circularly polarized at the highest URAP frequencies. New directional information provides crucial information on the effects of beamin...
Physics of Plasmas
We consider simultaneous oscillations of electrons moving both along the axis of symmetry and als... more We consider simultaneous oscillations of electrons moving both along the axis of symmetry and also in the direction perpendicular to the axis. We derive a system of three nonlinear ordinary differential equations which describe self-similar oscillations of cold electrons in a constant proton density background (np = n0 = constant). These three equations represent an exact class of solutions. For weak nonlinear conditions, the frequency spectra of electric field oscillations exhibit split frequency behavior at the Langmuir frequency ωp0 and its harmonics, as well as presence of difference frequencies at low spectral values. For strong nonlinear conditions, the spectra contain peaks at frequencies with values ωp0(n+m2), where n and m are integer numbers (positive and negative). We predict that both spectral types (weak and strong) should be observed in plasmas where axial symmetry may exist. To illustrate possible applications of our theory, we present a spectrum of electric field oscillations observed in s...
Coronal Disturbances, 1974
Properties of solar radio bursts observed by spacecraft at frequencies below several MHz are revi... more Properties of solar radio bursts observed by spacecraft at frequencies below several MHz are reviewed. In this frequency range most of the observed bursts are type III events (associated with particles) but several cases of type II emission (associated with shocks) have been reported. The analyses which lead to emission levels of type III solar bursts out to beyond 1 AU from the Sun also indicate that the low frequency radiation is observed at the harmonic of the emission region plasma frequency. Simultaneous particle and radio measurements imply that the bursts are generated near the leading edge of impulsive streams of solar electrons with energies extending from several hundred keV to several keV. Recent experiments measuring the direction of arrival of the radio emission allow the exciter particles to be tracked along the interplanetary magnetic field from regions near the Sun out to 1 AU.
Solar Physics, 1977
The first simultaneous observations of type III radio bursts using spacecraft separated by severa... more The first simultaneous observations of type III radio bursts using spacecraft separated by several tenths of an AU have been made using the solar orbiters HELIOS-A and-B. The burst beginning at 1922 UT on March 28, 1976, has been located from the intersection of the source directions measured at each spacecraft, and from the burst arrival time differences. Wide baseline observations give the radial distance of the source at each observing frequency. Consequently, coronal electron densities and exciter velocity were determined directly, without the need to assume a density model as has been done with single spacecraft observations. The separation of HELIOS-A and-B has also provided the first measurements of burst directivity at low frequencies. For the March 28 burst the intensity observed from near the source longitude (HELIOS-B) was significantly greater than from 60 0 W of the source (HELIOS-A).
Solar Physics, 2012
ABSTRACT
Twelve type 2 solar radio events were observed in the 2 MHz to 30 kHz frequency range by the radi... more Twelve type 2 solar radio events were observed in the 2 MHz to 30 kHz frequency range by the radio astronomy experiment on the ISEE-3 satellite over the period from September 1978 to December 1979. These data provide the most comprehensive sample of type 2 radio bursts observed at kilometer wavelengths. Dynamic spectra of a number of events are presented. Where possible, the 12 events were associated with an initiating flare, ground based radio data, the passage of a shock at the spacecraft, and the sudden commencement of a geomagnetic storm. The general characteristics of kilometric type 2 bursts are discussed.
Benson et al. (2015, this volume) selected 10 large magnetic storms, with associated Dst minimum ... more Benson et al. (2015, this volume) selected 10 large magnetic storms, with associated Dst minimum values less than or equal to -100 nT, for which high-latitude topside ionospheric electron density profiles are available from topside-sounder satellites. For these 10 storms, we performed a superposition of Dst and interplanetary parameters B, v, N(sub p) and T(sub p). We have found that two interplanetary parameters, namely B and v, are sufficient to reproduce Dst with correlation coefficient cc approximately 0.96 provided that the interplanetary parameter times are taken 0.15 days earlier than the associated Dst times. Thus we have found which part of the solar wind is responsible for each phase of the magnetic storm. This result is also verified for individual storms as well. The total duration of SRS (storm related structure in the solar wind) is 4 - 5 days which is the same as the associated Dst interval of the magnetic storm.
Long duration storms of type III radio bursts were discovered in the hectometer wavelength range ... more Long duration storms of type III radio bursts were discovered in the hectometer wavelength range during the last solar cycle, utilizing the RAE-1 satellite observations. The major results are discussed including the investigation of the average exciter speed, the density of the regions (streamers) in which they are produced, the degree of inhomogeneity of the medium and the solar wind speed. During the present solar maximum, the ISEE-3 radio experiment has provided a unique means of monitoring radio emissions in the interplanetary medium from about 10 to 215 solar radii, with an almost continuous time coverage. The authors review preliminary results of this analysis, including the correlation with the solar activity and with type I and type III storms.
Radio Physics of the Sun, 1980
We present simultaneous energetic electron and solar radio obser vations from the ISEE-3 spacecra... more We present simultaneous energetic electron and solar radio obser vations from the ISEE-3 spacecraft of several solar type III radio bursts, ^he UC Berkeley energetic particle experiment measures from 2 to ^ 10 keV with good energy and pitch angle resolution while the Meudon/GSFC radio experiment tracks type III radio bursts at 24 fre quencies in the range 30 kHz-2 MHz. Two types of electron events are observed by the particle experi ment: (1) the "normal" type of 20 to > 100 keV flare associated elec tron events reported previously, and (2) events where only electrons in the 2-10 keV range are observed. These low energy, 2-10 keV, elec tron events appear not to be associated with flares or high frequency (> 10 MHz) radio emission as reported in the Solar Geophysical Data bulletins, but rather they appear to be associated with individual type III bursts from low frequency type III storms. Both types of electron event are closely correlated to the very low frequency type III emission produced in situ at 1 A.U. The radio experiment is able to identify the direction of arrival of the radio emission through a combination of a dipole antenna spinning in the ecliptic plane plus z-axis antennas for out-of-the-ecliptic direction. The frequency of the radio emission pro duced in situ around the spacecraft can be identified by its omnidirec tional nature. We have compared the temporal behavior of the in situ radio intensity and the electron intensity. In every case good agree ment was found between the onset times for the in situ radio and elec tron events. For the single event where solar wind plasma density measurements were available the frequency of the radio emission is con sistent with the emission being generated at the second harmonic and not at the fundamental of the plasma frequency. We have made preliminary computations of the electron velocity distribution function parallel to the magnetic field, f(vjj), for several^events. In the > 20 keV events no strong positive slope ^ > 0 is observed, rather f(vj|) has a plateau-like shape, even dv |(311
Astronomy and Astrophysics, 1985
An analysis is presented of the system response of a satellite receiver-antenna system to locate ... more An analysis is presented of the system response of a satellite receiver-antenna system to locate a radio source when the satellite is tilted on its axis. The satellite is spin stabilized but experiences a tilt due to either a mechanical misalignment or a shift in the electrical axis caused by parasitic currents in other spacecraft structures. The shorter the antenna, the more significant the effects. Numerical techniques are developed for obtaining the Stokes parameters and the angular parameters of a uniform conical source sensed by a linear antenna in order to derive the average power response of a synthesized dipole to a point on a distributed polarized source. Relative gains are calculated along the antenna at different angles to the source. The techniques are applied to sample ISEE-3 satellite data for Type III solar radio bursts which were sensed by an axial and an equatorial antenna. The two antennas permit localization of the source and quantification of the polarization and...
General Assembly and Scientific Symposium, 2011
Geophysical Research Letters, 1996
We analyze 2f p radio emission observed during a perigee pass in August 1995 when the WIND spacec... more We analyze 2f p radio emission observed during a perigee pass in August 1995 when the WIND spacecraft was between 47 and 72 R E from Earth and upstream of the electron foreshock. The WAVES experiment on WIND measures the direction of arrival and complete polarization state of the 2f p radiation. We found no evidence for significant linear or circular polarization. For one period when we were able to utilize the direction finding capability to determine the actual 2f p source location, using an interplanetary shock as a diagnostic, the radio emitting region was confirmed to lie within the electron foreshock near the contact point. We indicate how such remotely observed 2f p emissions can be used to monitor the response of the electron foreshock to instantaneous changes in the interplanetary magnetic field.
Geophysical Research Letters, 1998
We discuss the thermal evolution of the spurion and messenger fields of ordinary gauge mediation ... more We discuss the thermal evolution of the spurion and messenger fields of ordinary gauge mediation models taking into account the Standard Model degrees of freedom. It is shown that for thermalized messengers the metastable susy breaking vacuum becomes thermally selected provided that the susy breaking sector is sufficiently weakly coupled to messengers or to any other observable field.
Geophysical Research Letters, 2001
The first simultaneous observations of type III radio bursts using spacecraft separated by severa... more The first simultaneous observations of type III radio bursts using spacecraft separated by several tenths of an AU have been made using the solar orbiters HELIOS-A and-B. The burst beginning at 1922 UT on March 28, 1976, has been located from the intersection of the source directions measured at each spacecraft, and from the burst arrival time differences. Wide baseline observations give the radial distance of the source at each observing frequency. Consequently, coronal electron densities and exciter velocity were determined directly, without the need to assume a density model as has been done with single spacecraft observations. The separation of HELIOS-A and-B has also provided the first measurements of burst directivity at low frequencies. For the March 28 burst the intensity observed from near the source longitude (HELIOS-B) was significantly greater than from 60 0 W of the source (HELIOS-A).
Two examples of type 2 radio emissions associated with the propagation of earth-directed coronal ... more Two examples of type 2 radio emissions associated with the propagation of earth-directed coronal mass ejections (CMEs) through the interplanetary medium are illustrated and compared. The two type 2 radio events were observed by WIND/WAVES in January and May of 1997 and exhibit very different radio characteristics. The analyses presented here use the novel approach of presenting the radio data as a function of the inverse of the frequency and time, which facilitates remote radio tracking of the CME through the interplanetary medium. It is demonstrated unequivocally that for the May 1997 event, the radio emissions were generated at the fundamental, and harmonic of the plasma frequency in the ambient plasma upstream of the CME-driven shock. For the January 1997 event, evidence is presented that some of the radio emissions were generated while the CME-driven shock passed through a corotating interaction region (CIR). This is the first time that type 2 radio emissions were shown to origi...
[
... radio experiment at ISEE 3, about one hour earlier in accordance with the transit time of ...... more ... radio experiment at ISEE 3, about one hour earlier in accordance with the transit time of ... However, these positions may have systematic errors if significant linear polarization is present in the observed ... Intensity variations of 20 db and apparent motions of 40 R E can occur with ...
The Ulysses URAP experiment has provided the first measurements of remote and in-situ wave phenom... more The Ulysses URAP experiment has provided the first measurements of remote and in-situ wave phenomena from high southern latitudes. Remote sensing of type 3 solar radio bursts constitute an important component of the Ulysses observations. Type 3 radio emissions, which have never before been viewed from outside the ecplitic plane, have been observed by Ulysses to its maximum southern latitude (approximately 80 deg S), although their frequency of occurrence has generally diminished due to the declining phase of the solar cycle. In addition, the Ulysses radio receiver measures both the direction of arrival and the complete polarization state of incident radiation. These physical parameters provide information on the origin and nature of the radio emission. Preliminary analyses have indicated that kilometric type 3 radiation is often approximately 10-20% circularly polarized at the highest URAP frequencies. New directional information provides crucial information on the effects of beamin...
Physics of Plasmas
We consider simultaneous oscillations of electrons moving both along the axis of symmetry and als... more We consider simultaneous oscillations of electrons moving both along the axis of symmetry and also in the direction perpendicular to the axis. We derive a system of three nonlinear ordinary differential equations which describe self-similar oscillations of cold electrons in a constant proton density background (np = n0 = constant). These three equations represent an exact class of solutions. For weak nonlinear conditions, the frequency spectra of electric field oscillations exhibit split frequency behavior at the Langmuir frequency ωp0 and its harmonics, as well as presence of difference frequencies at low spectral values. For strong nonlinear conditions, the spectra contain peaks at frequencies with values ωp0(n+m2), where n and m are integer numbers (positive and negative). We predict that both spectral types (weak and strong) should be observed in plasmas where axial symmetry may exist. To illustrate possible applications of our theory, we present a spectrum of electric field oscillations observed in s...
Coronal Disturbances, 1974
Properties of solar radio bursts observed by spacecraft at frequencies below several MHz are revi... more Properties of solar radio bursts observed by spacecraft at frequencies below several MHz are reviewed. In this frequency range most of the observed bursts are type III events (associated with particles) but several cases of type II emission (associated with shocks) have been reported. The analyses which lead to emission levels of type III solar bursts out to beyond 1 AU from the Sun also indicate that the low frequency radiation is observed at the harmonic of the emission region plasma frequency. Simultaneous particle and radio measurements imply that the bursts are generated near the leading edge of impulsive streams of solar electrons with energies extending from several hundred keV to several keV. Recent experiments measuring the direction of arrival of the radio emission allow the exciter particles to be tracked along the interplanetary magnetic field from regions near the Sun out to 1 AU.
Solar Physics, 1977
The first simultaneous observations of type III radio bursts using spacecraft separated by severa... more The first simultaneous observations of type III radio bursts using spacecraft separated by several tenths of an AU have been made using the solar orbiters HELIOS-A and-B. The burst beginning at 1922 UT on March 28, 1976, has been located from the intersection of the source directions measured at each spacecraft, and from the burst arrival time differences. Wide baseline observations give the radial distance of the source at each observing frequency. Consequently, coronal electron densities and exciter velocity were determined directly, without the need to assume a density model as has been done with single spacecraft observations. The separation of HELIOS-A and-B has also provided the first measurements of burst directivity at low frequencies. For the March 28 burst the intensity observed from near the source longitude (HELIOS-B) was significantly greater than from 60 0 W of the source (HELIOS-A).
Solar Physics, 2012
ABSTRACT