- Open Access
Magnetic alignment of nonmagnetic silicates caused by paramagnetic anisotropy: Origin of polarization observed in planetary formation region
© The Society of Geomagnetism and Earth, Planetary and Space Sciences, The Seismological Society of Japan 2010
- Received: 31 July 2008
- Accepted: 2 December 2008
- Published: 7 February 2015
Possible dust alignment in dense regions due to paramagnetic anisotropy ΔχPARA is discussed based on the results of a laboratory experiment on ortho-pyroxene grains containing a small amount of Fe2+ ions (1.8 mol%). Ortho-pyroxene has been detected in circum-stellar regions by infrared emission spectroscopy. Our experiment was performed at room temperature using He gas as the dispersing medium. Although the grains do not contain strong magnetic moments, alignment was achieved at low field strength (<2000 G). The alignment efficiency of ortho-pyroxene was compared with those of various rock-forming minerals. The magnitude of diamagnetic anisotropy ΔχDIA, free of paramagnetic ions, is generally <10-8 emu/g for various silicates. In contrast, ΔχPARA increases considerably with increasing Fe2+ concentration, reaching 10-5 emu/g for many of the silicates when the concentration of Fe2+ is >1 mol%; this increasing ΔχPARA is the cause of the above-mentioned alignment obtained at the low field strength. Based on our observations, we infer the field intensity needed to obtain partial dust alignment of sufficient size to explain the observed polarization in astrophysical environments. Due to temperature dependences caused by a Curie Law and a rotational Brownian motion, the field intensity required to cause the alignment is expected to decrease considerably at low-temperature conditions assumed for a proto-planetary disk. The results of our experiment performed at room temperature provide a technical basis to reproduce grain alignment under such temperature conditions.
- Magnetic field direction
- dust alignment
- ortho-pyroxene grains
- proto-planetary disks
- paramagnetic anisotropy
The direction of magnetic field B in a diffuse region is frequently estimated from infrared or visible polarization P caused by partial dust alignment; a weak galactic field of approx. 3 μG is considered to be the cause of alignment. Because the geometrical relationship between P and B strongly depends on the mechanisms of alignment, it is important to firmly establish this mechanism to obtain a reliable field direction from polarimetry data. The conventional mechanism of alignment (the so-called a “Davis- Greenstein model”) is based on a paramagnetic relaxation process of magnetic moments included in the dust (e.g. Spizer, 1978). This model requires an extremely high rotational energy relative to the thermal energy—a condition that is only met in a diffuse interstellar region. The model is not realistic for planetary formation regions wherein thermal equilibrium is achieved between dust and gas (Whittet, 1992). Consequently, alternative mechanisms for the origin of magnetic alignment should be considered for solid materials that do not possess a strong magnetic moment. According to data compiled on solar elemental abundance and infrared emission observational data, high concentrations of magnetic ions cannot be expected in the dust particles. The current theory of magnetic alignment of solid particles is that it occurs only for materials possessing a strong magnetic moment.
Alignment of micron-size crystals caused by the anisotropy of magnetic susceptibility Δχ was recently observed for common rock-forming silicates, namely kaolinite, talc, muscovite and biotite (Uyeda et al., 1991, 1993). The experiment was performed at room temperature (T = 300 K) using liquid ethanol as the dispersing medium. Partial alignment occurred by a simple balance between Brownian energy 1/2 kTBT and field-induced anisotropy energy 1/2 MΔB2, as was first proposed by Langevin and Curie (1910); where M denotes the mass of the particle and Δχ describes anisotropy per unit mass. This process of grain alignment has been quantitatively studied on inorganic material, such as clay and mica minerals (Uyeda et al., 1993, 2003, 2005a) where it was explicitly shown that alignment was controlled by Δχ, T and M. This result means that the minimum field intensity required to achieve alignment is predictable, provided that the numerical values of these three parameters can be determined. This mechanism of aligning nonmagnetic particles was considered to be a promising technique to develop new types of industrial material (e.g. Maret and Dransfield, 1985). When an axis of a grain material possesses high material functionality, such as in terms of hardness, conductivity or optical efficiency, among others, this functionality can also be preserved in a grain aggregate provided that the grain axes are orientated in one direction. Based on this principle, attempts were made to produce large single crystals of protein, synthetic bone materials or aggregations of carbon nano-tubes. However, to date, only a limited number of materials have been investigated. Alignment is believed to occur only at a field intensity >10,000 G, which requires a superconducting magnet.
Recent observations of infrared emissions have enabled the dust in the planetary formation region to be identified as rock-forming minerals, such as forsterite, ortho-pyroxene, diopside or hibonite; these are frequently observed in chondritic meteorites (e.g., Hanner et al., 1995; Malfait et al., 1998; Sitko et al., 1999; Honda et al., 2003; Hofmeister et al., 2003). The observations indicated that these silicates had Mg-rich components. Based on the observed 69-μm feature, the Fe concentration of the forsterite grains was estimated to be <5% (e.g. Molster et al., 2002). On the other hand, a small shift observed for the 11.44-μm feature of Vega-like star HD 14563 indicated the existence of Fe-bearing forsterite (Honda et al., 2004). Fe-bearing silicates are commonly seen in chondritic meteorites as well as in interplanetary dust particles (IDP) that are derived from the early solar system. It is likely that sufficient amount of silicate dusts in the circum-stellar region contain a small amount of Fe2+ ions (below several percent).
Here we report on an experimental study on the process of magnetic alignment. The experiment was carried out at room temperature on micron-sized ortho-pyroxene crystals dispersed in He gas, and the result was analyzed based on the Δχ values measured for bulk single crystals. Because temperatures of proto-planetary disks are estimated to range between T = 400 K and 50 K at a radius between 2 AU and 50 AU (Willacy and Langer, 2000), we discuss the effect of reducing the temperature on the magnetic alignment process. The practicability of dust alignment due to the above-mentioned process proposed by Langevin and Curie is quantitatively evaluated for the proto-planetary disks since reliable values of the three parameters are obtained for this region; values of T and M (dust size) are estimated from astronomical observation, whereas the Δχ value is determined by the magnetic-anisotropy measurement of a bulk single crystal composed of the same material as that identified in proto-planetary disks.
The bulk crystal sample was ground to a micron size and placed in the ampoule. The ampoule was connected to the sample chamber by a copper pipe. The interior of the chamber, the ampoule and the pipes were filled with He gas at 1.0 × 105 Pa. Thereafter, additional He gas was supplied to the ampoule at an enhanced pressure of about 1.1×105 Pa for about 1 s, and the sample grains were dispersed into the He gas. The gas with dispersed grains was injected into the chamber. The degree of grain alignment at arbitrary field intensity is obtained from the intensity of the He-Ne laser beam transmitted through the sample suspension in a direction parallel to the magnetic field. This can be done because the direction of an optical principle axis of a crystal grain coincides with the direction of the magnetic principle axis. The efficiency of the above method has been established in earlier experiments (Uyeda et al., 2001, 2003). A small portion of the dispersed grains was collected on a copper plate immediately after each experimental run was completed. M values at the time of the experiment were estimated as M = (1.9 ± 1.0) × 10-14 g, which was obtained from the size distribution (1.1±0.5 μm in diameter) observed on scanning electron microscope (SEM) images and volume density ρ = 3.2 g/cm3.
A theoretical fit to measured data is calculated from a Boltzmann average of 1/2(3 cos2θ - 1) in terms of a field-induced free energy of particle magnetic anisotropy Δχ is described as Δχ = χ‖ - χ⊥, where χ‖ and χ⊥ are the susceptibilities parallel and perpendicular to the stable axis, respectively. Here, a MΔχ value which gives the best fit to the measured data is used to describe the curves. The adopted MΔχ value in the above calculation was MΔχ = (4.3 ± 2.1) × 10-19 emu, which is consistent with the value obtained from the experimental M and ? values; MΔχ = (2.3±1.1)×10-19 emu. The consistency indicates that alignment proceeded by a Langevin process.
For the effect of Δχ, paramagnetic anisotropy ΔχPARA is a dominant factor compared to diamagnetic anisotropy ΔχDIA for most of the natural oxides. The origin of ΔχDIA was attributed to preferential orientation of bond direction with respect to a magnetic principle axis of crystal (Uyeda, 2004a). Accordingly, the ΔχDIA of various silicates was expected to distribute in a range between 10-8 and 10-10 emu/g. In contrast, ΔχPARA is derived from the anisotropy of the local crystalline field of a site that is occupied by an isolated paramagnetic ion (Ballet and Coey, 1982). Hence, ΔχPARA is proportional to the concentration of the paramagnetic ion; it reaches a level of 10-5 emu/g when the concentration of Fe2+ is about 1 mol%. Such concentrations of Fe2+ are often observed in major rockforming minerals. The effect of paramagnetic Fe2+ ions in reducing in Bs at room temperature was specifically observed for biotite grains, which is a typical sheet-silicate (Uyeda et al., 2005a). The value of Bs was found to be as low as 220 Oe for biotite, which had a susceptibility of χPARA = 4.4 × 10-5 emu/g. This Bs was less than 1% of the Bs value observed for synthetic phlogopite that was free of paramagnetic ions, whereas the Bs was 6.2 kOe for phlogopite with PARA = 1.2 × 10-6 emu/g. The concentration of Fe+2 is proportional to χPARA in the above three minerals. As almost equivalent crystal structures are reported for these minerals, they should have similar amounts of (Δχ)DIA. Hence, the large variation of Bs observed between the three materials can be attributed to the difference in the paramagnetic (Δχ)PARA.
Variations in the temperature are expected to change the values of (Δχ)PARA and Bs considerably since the paramagnetic moment follows a Cuire-Weiss law. The Δχ-T relationships were previously measured for bulk single crystals at between T = 300 K and 100 K for biotite and muscovite that contained Fe2+ ion at a level of 1 mol%. As temperature decreased from T = 300 K to 80 K, the Δχ of biotite increased from 1.2×10-5 emu/g to 8.0×10-5 emu/g, while the Δχ of muscovite increased from 0.9×10-6 emu/g to 5.1 × 10-6 emu/g (Uyeda et al., 2004b). The temperature dependence of Bs was measured between T = 300 K and 200 K for crystal grains of talc and kaolinite that contained paramagnetic ions (Uyeda et al., 2003). As shown in Fig. 3, observed Bs of kaolinite and talc was nearly proportional to T since (Δχ)PARA is proportional to T-1 following Curie’s law. Here, the magnitude of (Δχ)DIA was negligible compared to (Δχ)PARA. Hence, when a material contains a finite amount of paramagnetic ion, the reduction rate of Bs with decreasing T becomes much larger than the above-mentioned T½ dependence of a diamagnetic material. The measurement below T = 273 K involves using liquid ethanol as the dispersing medium; at the present time, pure water is used as the dispersing medium in most measurements.
In conclusion, most of the diamagnetic oxides have a potential to cause magnetic alignment, with the exception of cubic crystals and amorphous materials. The underlying reason for this is that the resultant Δχ may be enhanced considerably by increases in the concentration of paramagnetic ions. Δχ increases even more with decreasing temperature.
The values of χPARA, (Δχ)PARA and Bs observed for ortho-pyroxene are comparable to those of the biotite mentioned above. Consequently, Bs is expected to be considerably reduced in the low-temperature region below T = 100 K, which is now in progress for ortho-pyroxene. Precise measurements of both Δχ and Bs are required in the low-temperature region for ortho-pyroxene as well as for other dust minerals. These results may provide quantitative information that can be used to assess whether dust alignment in planetary formation region is caused by a simple Langevin process or not.
The magnetic field is known to be a major factor that controls the evolution of stars and planets. For example, reconnection of magnetic field associated with the protoplanetary disk was recently proposed to be a heat source that produces high-temperature condensates of primitive meteorites (Shu et al., 1997). In order to assess this hypothesis on planetary evolution, it is necessary to carry out high-spatial-resolution polarimetery mapping (about 1 AU). Near infrared (Lucas et al., 2004) and sub-millimeter (Tamura et al., 1999) imaging polarimetry was recently reported for YSO regions as well as for massive young objects (Momose et al., 2001). Spatial resolutions in these observations were about 100 AU although the data indicate that partial magnetic alignment of dust particles does take place in these systems. It is expected that polarimetry surveys with high-spatial resolution will be realized by forthcoming projects such as that of the Akatama Long Mand Association (ALMA).
It is necessary to reproduce the temperature conditions of planetary formation regions, which range between 400 K and 50 K; the setup shown in Fig. 1 is a step towards realizing alignment in a temperature range between T = 200 K and 50 K. In addition, our apparatus is capable of performing magnetic alignment in a reduced temperature condition down to T = 10 K, which is comparable to that of the molecular cloud. The experiment was possible because He gas is a unique medium that can disperse micron-sized particles and remain in the liquid state above T = 4.2 K. At the present time, measurements are only possible at temperatures above 160 K for silicate grains since liquid ethanol is used as a dispersing medium. As mentioned before, it is essential to know the geometrical relationships between B and P for determining the field direction from polarimetry data. This relationship differs considerably depending on the alignment model used. The apparatus shown in Fig. 1 is capable of examining the relationship between P and the direction of the crystalline axes of mineral grains, which is not clearly understood in the dense region.
The authors wish to thank Dr. Anne Hofmeister for valuable comments and discussions.
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