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Attempt to detect diamagnetic anisotropy of dust-sized crystal orientated to investigate the origin of interstellar dust alignment
Earth, Planets and Space volume 65, Article number: 8 (2013)
Diamagnetic anisotropy Δχ dia was detected on a submillimeter-sized calcite crystal by observing the rotational oscillation of its magnetically stable axis with respect to the magnetic field direction. The crystal was released in an area of microgravity generated by a 1.5-m-long drop shaft. When the oscillations are observable, the present method can measure Δχ dia of crystal grains irrespective of how small they are without measuring the sample mass. In conventional Δ χ measurements, the background signal from the sample holder and the difficulty in measuring the sample mass prevent measurement of Δχ dia for small samples. The present technique of observing Δχ dia of a submillimeter-sized single crystal is a step toward realizing Δχ dia measurements of micron-sized grains. The Δχ dia values of single micron-sized grains can be used to assess the validity of a dust alignment model based on magnetic torque that originates from the Δχ dia of individual dust particles.
The spatial distributions of inter- and circumstellar magnetic fields are commonly estimated from the polarization of visible and infrared light from stars; this polarization is considered to result from the magnetic alignment of the dust particles that are present in various regions (e.g. Spizer, 1978). The origin of grain alignment in the diffuse interstellar region had been explained by a paramagnetic relaxation of the grains; here the grain possesses angular momentum due to its collisions with the gas particles (Davis and Greenstein, 1951). The model was improved by assuming a spin-up of the grain caused by the ejection of molecular hydrogen from the grain surface (the “pinwheel mechanism”, Purcell, 1979), however quantitative inconsistencies remained between the improved model and observed interstellar conditions (e.g. Lazarian and Draine, 1999). A possibility of grain alignment based on a radiative torque was proposed (Dolginov and Mitrofanov, 1976); the torque was effective on irregularly-shaped grains with geometrical “helicity”. The efficiency of the radiative torque was improved by assuming super-paramagnetic inclusions in the grains (Lazarian and Hoang, 2008). The magnetic properties were studied for metallic inclusions formed in various types of silicate matrix (Djouadi et al., 2007); their microstructures resembles those of glass with embedded metal and sulphides found in the interplanetary dust particles. Large remnant magnetization that derives from magnetic inclusions contained in natural olivine crystals are reported (Belley et al., 2009); olivine is recognized as one of the major minerals contained in meteorites and circumstellar dusts. It was pointed out that the large magnetizations of these materials are effective in realizing grain alignment in terms of the above-mentioned mechanisms (Djouadi et al., 2007). In high-density regions, the mechanism of dust alignment is still unclear, because the effects of the above-mentioned mechanism are reduced when dust is in thermal equilibrium with the gas medium (Whittet, 1992).
A simple mechanism has been proposed that is based on the balance between the rotational Brownian energy and the magnetic anisotropy energy of a dust particle. Unlike the conventional models, this mechanism is effective even when gas and dust are in a thermal equilibrium state. The magnetic anisotropy may be caused by paramagnetic anisotropy Δ χ para and/or by diamagnetic anisotropy Δχ dia (Uyeda et al., 1991, 1993). The amount of Δ χ para required for dust alignment has been quantitatively discussed based on laboratory experiments using orthopyrox-ene grains containing a low concentration (~1 mol.%) of Fe3+ ions; orthopyroxene has been detected in circumstel-lar regions by infrared emission spectroscopy (Honda et al., 2003). Since the temperature dependence of Δχ para follows the Curie law, the field intensity required to cause alignment is expected to be relatively low at the low temperatures that are assumed to exist in the outer regions of proto-planetary disks (Uyeda et al., 2003a, 2005). Correlation between interstellar polarization and dust temperature was confirmed for 14 lines of sight towards the Pleiades cluster (Matsumura et al., 2011), which was compatible with an alignment model based on the radiative torques. The observed correlation between temperature and polarization is effective to examine the efficiency of the above-mentioned models based on magnetic torques, since large temperature dependences are expected for the magnetizations of dust materials (Uyeda et al., 2003a; Belley et al., 2009).
In diffuse clouds, the concentrations of magnetic ions in the dust particles are considered to be too low to cause dust alignment. In these regions, dust alignment may be caused by Δχ dia (Chihara et al., 1988; Uyeda et al., 2003b). According to a recent model based on experimental Δχ dia data, materials generally possess an intrinsic Δχ dia . Recently, there have been various attempts to determine the effective susceptibility of a small diamagnetic particle. Significant increases in Δχ dia with decreasing crystal size have been reported recently for various materials. To assess the validity of the above-mentioned alignment model, it is essential to obtain the effective Δχ dia of actual dust particles. However, it is difficult to determine Δχ dia using conventional methods for samples with submillimeter diameters. In the present study, Δχ dia of submillimeter calcite crystals was obtained for the first time by measuring the period of rotational oscillations caused by the field-induced anisotropy energy. The crystals were released in a microgravity (μG) area generated by a short drop shaft. The size dependence of Δχ dia is then investigated using calcite crystals of different sizes. The possibility of extending these measurements to micron or submicron sizes is discussed based on the obtained results.
In the present study, μG conditions were produced using a 1.5-m-long drop shaft, which was designed and constructed at the Graduate School of Science, Osaka University. The drop shaft produced μG for a duration of 0.5 s. An experimental setup developed to measure magnetic rotation was installed in the drop shaft. It was in the form of a rectangular box that had internal dimensions of 35 cm × 30 cm × 20 cm. Routine μG experiments using the above-mentioned short drop shaft were difficult for larger box sizes. Prior to the experiment, submillimeter calcite crystals were inserted in the center of a homogeneous field generated by a magnetic circuit consisting of two NdFeB magnetic plates with dimensions of 2.5 cm × 2.0 cm × 0.6 cm. The magnetic field intensity at the center of the circuit was 0.63 T. The sample was supported by a sample stage. The calcite crystals were cut from a high-quality natural single crystal (Ecke, Iceland). Magnetic and chemical analyses performed in a previous study (Uyeda et al., 1993) revealed that it had a paramagnetic ion concentration of less than 1 ppm. The published Δχ dia value of calcite is 4.05 × 10−8 emu/g and the crystal c-axis is a magnetically unstable axis (Uyeda et al., 1993). The experimental setup was enclosed in a vacuum chamber that had Pyrex walls to allow the sample motion to be observed from outside by a high-vision video camera (Panasonic, HDC-SD3-S) that had time and spatial resolutions of 0.033 s and 0.004 cm, respectively.
The drop box was attached to the laboratory ceiling. About 0.05 s after the beginning of μG, the sample was released from the sample stage in the homogeneous field region with a negligibly small angular momentum. The low pressure of the medium in the chamber (P ≈ 100 Pa) resulted in a low viscous drag. Prior to performing the μG experiments using the chamber drop shaft, operational tests of the above-mentioned setup were conducted to observe oscillation in a drop shaft at the National Institute of Advanced Technology AIST, which had a μG duration of 1.35 s and a residual gravitational acceleration of below 50 Gal. These tests confirmed that images of rotational oscillation could be recorded within a time 0.5 s (i.e., the μG duration of the chamber drop shaft).
3. Results and Discussion
In the present study, a diamagnetic single crystal is released in a low-pressure μG area with a homogeneous magnetic field B and the initial angular momentum of the sample is negligibly small. Under these conditions, the magnetically stable axis causes rotational motion with respect to B. The rotation obeys
where θ denotes the angle of the stable axis with respect to B; I is the moment of inertia of the crystal. When the initial value of θ is sufficiently small, the period of rotational harmonic oscillation of the crystal can be written as:
When the values of B and Im−1 are known, the above equation can be used to determine the intrinsic Δχ dia of the material, only by measuring τ. The sensitivity of measuring a small Δχ dia can be improved by increasing B and/or by increasing τ. Using the above equation, the τ values of various millimeter-sized samples were measured to obtain their Δχ dia (Uyeda et al., 1993, 2005).
In the present study, calcite crystals underwent rotational oscillation with the geometry shown on the right-hand side of Fig. 1. In these oscillations, the equilibrium direction of the crystal c-axis was perpendicular to the field, since the c-axis was the magnetically unstable axis. The values of τ and Im−1 of the crystal were estimated from the images obtained using the high-vision camera. As mentioned before, the value of B was 0.63 T in the homogeneous area of the circuit. By substituting these three values into Eq. (2), the Δχ dia of a single crystal grain can be obtained. Rotational oscillations of five calcite crystal grains with different masses m were measured. Table 1 lists the obtained values of τ, Δχ dia and m. Whereas, Fig. 2 shows a plot of Δχ dia against m. No significant dependence of Δχ dia on m is observed for calcite above the experimental error. This mass independence is expected from Eq. (2). To quantitatively examine the slight enhancement of Δχ dia on reducing m, it is essential to improve the accuracy of Im−1 values to reduce the experimental errors in Fig. 2. Submillimeter samples are not expected to show a significant increase in Δχ dia with decreasing size.
It has been considered that circumstellar magnetic fields play a major role in the evolution of protoplanetary disks. To quantitatively examine the validity of various models on disk evolution based on the magnetic field, it is necessary to accurately measure the polarimetric distribution with a high spatial resolution. Near-infrared imaging polarimetry has been performed for massive young objects (Momose et al., 2001). In addition, young stellar objects have been imaged by near-infrared (Lucas et al., 2004) and submillimeter (Tamura et al., 1999) imaging of polarization. It is expected that a polarimetry survey with a high spatial resolution is realized by an Atacama Large Millimeter Array project. As mentioned above, it is essential to determine the dust alignment mechanism to obtain reliable field directions from polarimetry data, because the dust alignment mechanism determines the relationship between the magnetic field direction and the polarization. As mentioned before, the alignment mechanism based on relaxation of the paramagnetic moment of dust is not quantitatively approved, as yet, in the planetary formation regions where dust and gas are in thermal equilibrium (Whittet, 1992). The high angular momentum relative to that of the thermal equilibrium state assumed in the mechanism is realized only in diffuse interstellar regions. Hence, an alternative model was proposed that describes the origin of magnetic alignment based on the anisotropy of magnetic susceptibility (Uyeda et al., 2003b, 2010).
Magnetic alignment of diamagnetic particles has received much attention in connection with the processing of functional materials (e.g. Maret and Dransfield, 1985); an aggregate of grains with their crystal axes oriented in a single direction is expected to realize additional functionality along the oriented direction. The alignment process has been qualitatively analyzed by assuming a balance between the anisotropy energy, 1/2mΔχB2, and the rotational Brownian motion, 1/2k B T; here, Δ χ denotes magnetic anisotropy (Δχ para and/or Δχ dia ). In order to estimate the field intensity required to achieve alignment, a new parameter (B s ) was proposed to describe an ensemble of diamagnetic particles dispersed in a liquid medium at temperature T (Yamagishi et al., 1989). B s is defined as the field intensity at which the order parameter 〈M〉 ≈ 0.78, where 〈M〉 is the average value of the function 1/2(3 cos2θ − 1) for a grain ensemble. In the above function, θ is the angle between the magnetically stable axis of a grain and B. The value of B s was directly calculated for a Langevin process (Langevin and Curie, 1910) to be
This equation indicates that B s decreases with decreasing T and with increasing m or Δχ. The theoretical value of B s is typically calculated by substituting experimentally measured m, Δχ, and T values into Eq. (3), while an experimental estimate of B s is independently obtained from the measured 〈M〉 − B relationship. When these two values of B s agree with each other, the grain alignment is considered to be driven by a Langevin process. The above-mentioned agreement was examined for various minerals contained in meteorites and circumstellar dust (Uyeda et al., 2005a, 2010), and the possibility of grain alignment caused by Δχ para was discussed on the basis of the agreement.
The dust alignment caused by Δχ dia is considered to be less realistic compared with an alignment caused by Δχ para , since the calculated B S value based on Δχ dia , obtained by bulk crystal measurement, is considerably large compared to the astronomical magnetic field. As mentioned before, significant increases of Δχ dia with decreasing crystal size was reported recently for some of the ceramic materials. If the diamagnetic anisotropy energy due to the enhanced Δχ dia of the micron-sized material becomes comparable to the Brownian motion energy at an astronomical condition, partial alignment of dusts may occur by Δχ dia . Unlike many of the conventional models that are based on super-thermal effects, the mechanism based on diamagnetic anisotropy energy is effective in the dense region where the evolution of proto-planetary discs take place. Furthermore, the mechanism is free of various specific magnetic-structures assumed in the previous models; the magnetic-structures were composed of small magnetic inclusions.
The practicability of considering grain alignment by diamagnetic anisotropy energy can be examined, by evaluating the quantitative amount of Δχ dia enhancement at the micron-size level. The new method for measuring Δχ dia in μG conditions, as described in Fig. 1, is free of a restoration torque since the sample is not suspended by a fiber. Furthermore, the method does not require measuring the sample mass. These two factors limit the minimum sample size of conventional methods for measuring Δχ dia under normal gravity. This implies that the present method, based on the observation of rotational oscillation, can measure the diamagnetic anisotropy of samples irrespective of how small they are. The minimum sample size could potentially be of the order of nanometers if an ultraviolet fluorescence microscope is introduced in the drop box. In the above setup, the sample rotation is observed by the ultraviolet emission from a fluorescent bead that is attached to the sample. The minimum diameter of this bead is presently several nanometers. Hence, Δχ dia is measurable for a particle that has a diameter greater than 10 nm. As a step toward realizing measurements at μ m and nm scales, it is important to improve the accuracy of Im−1 measurements of submillimeter samples (see Fig. 2). The demand for measuring Δχ dia of small single particles is increasing due to the growing interest in nano-sized materials in various research fields. Finally, the present experimental system to observe the free magnetic rotation of a single particle is applicable to examine the effectiveness of various types of magnetic torques that has been proposed in the conventional models to explain dust alignment. In order to perform these examinations, it is essential to realize the above-mentioned observation for micron and submicron sized particles.
When the period of field-induced rotational oscillation τ is observed for a crystal that is subject to μ G conditions, its diamagnetic anisotropy Δχ dia (per unit mass) can be measured for any crystal, no matter how small they are. This is because the method does not require a sample holder and does not need to measure the sample mass.
By employing a compact drop shaft that produces μ G conditions for 0.5 s, Δχ dia was detectable for submillimeter calcite crystals by measuring τ. No significant mass dependence was observed for the Δχ dia values at this size.
The validity of a dust alignment model based on diamagnetic anisotropy is quantitatively examined by obtaining mΔχ dia values at sizes equivalent to those of dust particles. This is because the field intensity to achieve alignment is uniquely determined by mΔχ dia of the dust and the medium temperature T. We are currently seeking to improve these Δχ dia measurements under μ G conditions to enable Δχ dia to be measured for micron-sized crystals.
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Takeuchi, T., Hisayoshi, K. & Uyeda, C. Attempt to detect diamagnetic anisotropy of dust-sized crystal orientated to investigate the origin of interstellar dust alignment. Earth Planet Sp 65, 8 (2013). https://doi.org/10.5047/eps.2012.05.007
- Dust alignment
- diamagnetic anisotropy
- magnetic rotational oscillation