1. (University of Texas at El Paso) (New Mexico State University at Doña Ana) Radio Observations of Cataclysmic Variables Paul A. Mason (University of Texas at El Paso) (New Mexico State University at Doña Ana) With thanks to Collaborators: S. Howell (NOAO) T. Harrison (NMSU) K.P. Singh, V. Girish (TIFR-Mumbai) Saika (NCRA-GMRT) M. Claussen (NRAO)

2. Radio Surveys (see Mason and Gray ApJ, 2007 for a detailed review) Surveys of non-magnetic CVs have not found any persistent radio sources. AM Her and AE Aqr were discovered to be radio emitters early in the process of surveying magnetic CVs. (e.g. Chanmugam, and Dulk, 1982). Nearly all of the pre-ROSAT magnetic CVs were observed and found not to be radio emitters. (e.g. Beasley et al. 1994; Mason, Fisher and Chanmugam 1996). AR UMa was discovered to be a persistent radio source in a recent survey (Mason and Gray, 2007). Note: The reported discovery of a CV from radio data, FIRSTJ1023, is actually a pulsar (Thorstensen)..

3. Radio Studies Despite decades of searching, there are only 3 persistent radio CVs, but there is also a radio emitting pre-CV, V471 Tau. AR UMa (highest field known for a polar, 230 MG AM Her (prototype polar low (13 MG) field AE Aqr (magnetic propeller Intermediate Polar) V471 Tau (detached wind accreting pre-magnetic CV) So what do these 4 binaries have in common?

4. Isolated Magnetic WDs are not radio sources Holberg, Oswalt, and Sion (2002) compiled a list of 109 white dwarfs whose best distance estimates place them within 20 pc of the sun. This includes two binary white dwarfs. They state that the sample is likely to be complete out to 13 pc and is 65% complete to 20 pc. Liebert, Bergeron, and Holberg (2003) examined a subset of 11 magnetic white dwarfs within 20 pc. None of these are radio sources. These white dwarfs cover a range of magnetic field strengths from ~0.2 to 320 MG. The radio flux density from a magnetic white dwarf at 13 pc would be a factor of 50 times as great as that detected from AR UMa Radio Studies Isolated Magnetic WDs are not radio sources Holberg, Oswalt, and Sion (2002) compiled a list of 109 white dwarfs whose best distance estimates place them within 20 pc of the sun. This includes two binary white dwarfs. They state that the sample is likely to be complete out to 13 pc and is 65% complete to 20 pc. Liebert, Bergeron, and Holberg (2003) examined a subset of 11 magnetic white dwarfs within 20 pc. None of these are radio sources. These white dwarfs cover a range of magnetic field strengths from ~0.2 to 320 MG. The radio flux density from a magnetic white dwarf at 13 pc would be a factor of 50 times as great as that detected from AR UMa

5. Isolated fast rotating red dwarf flare stars cannot account for the persistent radio flux density seen in AM Her and AR UMa So a binary with a magnetic WD is necessary, but observations of V471 Tau as well as low states of AM Her and AR UMa show that radio emission does not require high-state accretion. Radio Studies Isolated fast rotating red dwarf flare stars cannot account for the persistent radio flux density seen in AM Her and AR UMa So a binary with a magnetic WD is necessary, but observations of V471 Tau as well as low states of AM Her and AR UMa show that radio emission does not require high-state accretion.

6. Radio Flare From SS Cyg (Körding et al. 2008). Is it a synchrotron jet?

7. Multiwavelength campaign AR UMa Phased-resolved VLA 6hr light-curve @ 3.6 cm Snapshots @VLA 3.6cm, 6cm, 20cm GMRT 50cm UBVRI Photometry NMSU 1m Tom Harrison Optical Spectra 2hr WYNN Steve Howell

8. GMRT: Giant Metrewave Radio Telescope near Pune, India, is currently the largest operating array dedicated primarily to observations in the 21 cm to 6 m wavelength range.

9. GMRT The design of the GMRT array resembles that of the VLA. Its field of view is determined by the diffraction limit of one 45-m antenna.

10. Phase resolved B, V, and I light curves of AR UMa obtained March 9 th 2008 Orbital Phase AR UMa was in a low state during the GMRT Observations

11. High State Comparison Spectrum AR UMa “Sleeping”

12. AR UMa ---- VLA 6 hours --- covering 3 Orbital Cycles

13. Phase Resolved 8.4 MHz Light Curve of AR UMa Orbital Phase

14. GMRT 50cm map of AR UMa Detected during a very low accretion state

15. Ultra-relativistic electrons in Jupiter's radiation belts (Bolton et al. 2002)

16. Charged particles, especially electrons, get trapped in Jupiter's magnetosphere. Electrons spiral along magnetic field lines bouncing back and forth between the magnetic poles by the well known magnetic mirror effect. There must be a supply of electrons injected into Jupiter's magnetosphere and there must be a way to accelerate these electrons to MeV energies. An additional observation clarifies how this might occur. There is a correlation between the Solar UV flux and the JSR. Both criteria may be realized if enhanced solar UV flux causes the upper atmosphere of Jupiter to expand by heating, resulting in a partially ionized wind. As the partial plasma expands into the magnetosphere of Jupiter, neutral atoms impede the flow of protons while the electrons move forward. The separation of the electrons from the protons set up strong electric fields which accelerate the electrons to Mev energies. These fast moving electrons become trapped in Jupiter's magnetosphere and dissipate their energy as Synchrotron radiation. Neutral Wind Dynamo

17. A very similar mechanism may be working in the magnetosphere of the secondary of AR UMa, which likely has a wind as evidenced from HST observations. A significant difference is of course the strong magnetic field of the white dwarf in AR UMa. It might be more proper to say the combined primary and secondary magnetosphere of AR UMa. A determination of the position and SED of radio emission will place models on mechanisms

18. From HST STIS Observations of AR UMa Gänsicke et al. (2001) found P-Cygni profiles that they attribute to a wind from the trailing face of the secondary.

19. Future Prospects The VLA is currently being retrofitted with new receivers, correlators, and electronics. The Extended Very Large Array (EVLA) is essentially a new telescope using the VLA dishes. Its will have its bandwidth increased by a factor of 80 and will increase continuum source sensitivity by a factor of 5-20 depending on the frequency. Future Prospects The VLA is currently being retrofitted with new receivers, correlators, and electronics. The Extended Very Large Array (EVLA) is essentially a new telescope using the VLA dishes. Its will have its bandwidth increased by a factor of 80 and will increase continuum source sensitivity by a factor of 5-20 depending on the frequency.

20. AM Her and AR UMa have similar flux densities and distances. By scaling the radio flux density of these polars, the EVLA will be able to detect radio CVs out to 500pc.

21. Is there a future in radio observations of CVs?

22. VLBA will provide the first spatially resolved observation of any CV