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5.1. Basic detection concepts at Radio, Extreme IR, Far IR, and Mid IR Wavelengths

How can we detect from Earth the distant interstellar magnetic fields ? Special particles affected by the magnetic field near them will emit a tell-tale polarized signal which we can capture on Earth. Thus by rotating a polarimeter attached to a radio telescope on Earth, we can detect this tell-tale polarized signal.

Figure 7 shows that high-energy relativistic electrons are trapped inside magnetic flux tubes or magnetic pipelines, in which the electrically-charged particles can glide along the lines by spiralling around them. While spiralling, they emit a synchrotron radio wave with its E-vector polarized in a direction perpendicular to the magnetic flux tube, and it is often emitted strongly at centimeter and meter wavelengths.

Figure 7

Figure 7. High-energy relativistic electrons are trapped by a magnetic field and forced to orbit around the field line. A plaintive synchrotron (non-thermal) signal from a trapped relativistic electron is emitted strongly at meter and centimeter wavelengths.

Figure 8 shows dust grains trapped and aligned by a magnetic field. Dust grains do emit a thermal continuum emission. The needle-like grain turns end-over-end around its center, akin to a pirouette; here the grain's short axis of rotation is aligned along the magnetic field line as proposed by some grain alignment theories - other grain alignment theories predict the grain's long axis to be aligned along the magnetic field line (e.g., Lazarian et al. 1997). The grain emits primarily in the plane of the rotation/pirouette, and its E-vector emission is polarized in a direction parallel to the grain's long axis, hence here perpendicular to the magnetic field lines. The signal is emitted strongly at Extreme IR wavelengths and at Far Infrared wavelengths.

Figure 8

Figure 8. Elongated dust grains are aligned by an ambient magnetic field and forced to spin around the field line. A plaintive (thermal) signal from a trapped dust grain is emitted strongly at millimeter and submillimeter wavelengths.

Original unpolarized background optical stellar light is mostly absorbed by dust if the photon's E-vector is in the plane of the grain's long axis, and mostly transmitted if the photon's E-vector is in the plane of the grain's short axis, so at optical and near Infrared wavelengths we observe more optical photons with their E-vectors parallel to the ambient magnetic field lines.

Expressing the Planck function in the optically thin régime, one gets

Equation 8

where Omega in steradians is the solid angle of the source as seen from the Earth, h is the Planck constant, and c is the speed of light and tau is the "optical" depth at frequency nu, where

Equation 9

with Qlambda is the grain emissivity, a in cm is the grain radius, rho in g cm-3 is the grain density, Md / Mg approx 0.01 is the dust mass to grain mass in a cubic centimeter, and NH2 in cm-2 is the column density of molecular hydrogen, and Qlambda = 3.8 × 10-4[250 / lambda]2 , with lambda in microns.

Hildebrand (1983) has reviewed the derivation of dust characteristics and cloudlet masses from submillimeter/Extreme IR thermal emission, independent of grain models. He found that the dust mass Md = (4/3)[a rho / Qnu][Snu D2 / Bnu, T], where Snu is the flux density at frequency nu, D is the distance from the Earth to the source, Bnu, T is the Plank function with frequency nu and temperature T, Qnu is the grain emissivity at frequency nu, a approx 0.1 µm is the grain radius, rho is the grain density. Typically the value arho ~ 2.8 × 10-5 g cm-2, and the value (4/3)[arho / Qnu] ~ 0.1 g cm-2 , at lambda = 250 µm. Hence one derives:

Equation 10

where nu is in TeraHertz and T is the dust temperature (e.g., Little et al. 1990). For an early review, see Heiles et al. (1991).

In addition, the first detection of a linearly polarized (non-masing) molecular line has been obtained with the 15m James Clerk Maxwell Telescope (JCMT) in CO 2-1 (230 GHz, lambda1300 microns) (e.g., Greaves et al. 1996). This is a potentially useful probe of magnetic field as predicted earlier (e.g., Kylafis 1983). Here the percentage of linear polarization reaches a maximum for an 'optical' depth near 1 but it does not depend on the strength of the magnetic field. Also, the polarization position angle can be independent of the magnetic field direction (for a weak magnetic field) or else either parallel or pendicular to the magnetic field direction (for a strong magnetic field >> 1 microGauss). Glenn et al. (1997b) also detected ~ 0.8% linear polarization at PA ~ - 70° in CS 2-1 (near lambda3000 µm), but attributed this amount of polarization entirely to the elongation of the envelope of the giant branch star IRC+102216; they also claimed that the magnetic field there is either negligible or else is weak (<< 2 mGauss) and radially directed by the stellar wind.

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