Download PDF by J. Trujillo-Bueno, F. Moreno-Insertis, F. Sanchez: Astrophysical Spectropolarimetry

By J. Trujillo-Bueno, F. Moreno-Insertis, F. Sanchez

ISBN-10: 0521809983

ISBN-13: 9780521809986

This ebook includes the lectures brought on the XII Canary Islands iciness tuition of Astrophysics on Astrophysical Spectropolarimetry. It highlights how fresh advancements in theoretical astrophysics and astronomical instrumentation are major an ever-growing variety of astrophysicists to understand the big diagnostic capability provided via spectropolarimetry.

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Sample text

8. The electric field is given in arbitrary units. Time is given in units of the period T of the circular motion. it is found that synchrotron radiation is strongly linearly polarized (typical values of the fractional polarization being of the order of 75%), the direction of polarization being perpendicular to the magnetic field. 15. Polarization in spectral lines In the spectropolarimetric analysis of several astrophysical objects, it is commonly observed that spectral lines are polarized, the polarization signature being, in general, different from line to line and variable along the line profile.

The atom thus results in being pumped only in the two sublevels Mu = 1 and Mu = — 1, which entails the presence of atomic polarization in the upper level. The situation is schematically illustrated in Fig. 16a, the number of dots drawn on each sublevel being proportional to its population. The figure shows that in this case the atom is strongly polarized. When a polarized atom de-excites, the radiation emitted is, in general, also polarized. To find its polarization properties, it is enough to take into account that a quantum E.

Synchrotron Radiation As we have seen in the former section, a non-relativistic electron (or any other charged particle) moving in a constant magnetic field describes a helical trajectory characterized by the frequency we- At he same time, the electron radiates a monochromatic wave of the same frequency and with the polarization characteristics described above. For relativistic particles, the physical characteristics of the motion of the electron remain the same, except that the cyclotron frequency is changed into a lower frequency (now depending on the velocity of the particle), called the synchrotron frequency and defined by e0B ws = where 7, the Lorentz factor, is given by with (3 = v/c.

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Astrophysical Spectropolarimetry by J. Trujillo-Bueno, F. Moreno-Insertis, F. Sanchez

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