• ISAS Small Science Program
  • JSPS Scientific Research(S)

ISAS Small Science Program: DUST (Determining Unknown yet Significant Traits)

Working Group: DUST Nucleation
Term of Project: FY 2017-2022

PI: Yuki Kimura (Hokkaido University)

Great objective

Elucidate a whole processes of material evolution from molecules, dust, planet and to organics in a history of the universe based on fundamental physical and chemical properties of dust.

Why cosmic dust?

“Most of the atoms in the interstellar medium exist in the gas phase. Only about 1% of the total mass of the elements forms tiny solid particles called grains. Despite their low abundance, these grains are significant as building blocks of planetary systems, as substrates for the formation of molecules, as energy transducers in interstellar and circumstellar environments, and as key players in the efficient formation of stars. The efficiency of these various contributions depends strongly on the chemical composition, size, crystal structure, and geometry of the grains that are initially formed in gaseous outflows of evolved stars and subsequently processed in interstellar environments. Therefore, to understand these characteristics of grains, it is necessary first to clarify the compositions and quantities of grains formed in stellar gas outflows.” (Reference: Y. Kimura,* K. K. Tanaka, T. Nozawa, S. Takeuchi, Y. Inatomi, Pure iron grains are rare in the universe, Science Advances, 3 (2017) e1601992)

Scientific goal of this project is determined most important physical properties (surface tension and sticking probabilities) and infrared spectra during formation and agglomeration of cosmic dust under microgravity condition.

Elucidation of formation processes of silicate dust

Silicates has been distributed ubiquitously in the universe and also main minerals on the Earth and, therefore, understanding its formation process are very much important.  We will determine two crucial physical parameters, sticking probability of molecules and surface free energy by means of interferometry (Figures 1-3), and obtain infrared spectra (Figure 4) during formation of silicate dust by microgravity experiments.

Figure 1.  A photograph of the double wavelength Mach–Zehnder-type laser interferometer with an evaporation chamber.  Red and green arrows show the optical path.  (Reference: Y. Kimura,* K. K. Tanaka, T. Nozawa, S. Takeuchi, Y. Inatomi, Pure iron grains are rare in the universe, Science Advances, 3 (2017) e1601992.)
Figure 2.  A still snapshot of in-situ observation of the interference fringe during after smoke nanoparticles formed via homogeneous nucleation under (a) gravity and (b) micro gravity conditions.
Figure 3.  The surface free energy (s) against the sticking probability (a) obtained by the simulations using the semi-phenomenological nucleation model to explain the nucleation temperature (solid line) and size of the resulting particles (dashed line) observed in the experiment. (Reference: Y. Kimura,* K. K. Tanaka, H. Miura, K. Tsukamoto, Direct observation of the homogeneous nucleation of manganese in the vapor phase and determination of surface free energy and sticking coefficient, Crystal Growth & Design, 12 (2012) 3278–3284.)
Figure 4.  Originally designed experimental system for measurement of infrared spectrum of free flying nanoparticles during nucleation and growth in gravity environment.  (Reference: S. Ishizuka, Y. Kimura, T. Yamazaki, T. Hama, N. Watanabe, A. Kouchi, Two-step Process in Homogeneous Nucleation of Alumina in Supersaturated Vapor, Chemistry of Materials, 28 (23) (2016) 8732–8741.)

Elucidation of formation processes of carbonaceous dust

Determine the physical parameters of carbon and titanium carbide (TiC) dust and elucidate formation condition of core-mantle dust (Figure 5) is an objective of this project.  It is still difficult to explain the thickness of the graphitic mantle layer based on the typical physical conditions expected in the circumstellar envelopes of carbon stars (Reference: Lodders & Fegley 1995; Sharp & Wasserburg 1995; Chigai et al. 2002); T. Chigai, T. Yamamoto, C. Kaito & Y. Kimura, ApJ, 587 (2003) 771.).  Infrared spectrum of TiC makes a strong constrain on the origin of 21 mm feature of C-rich star (Figure 6).

Figure5.  Examples of core-mantle dust founding a meteorite.  Carbonaceous dust contains carbides of titanium, zirconium, molybdenum and/or ruthenium.  (Reference: Croat, et al. Astrophys. J.631 (2005) 976.)
Figure6.  Infrared spectra of post-asymptotic giant branch star SAO 96709 observed by ISO (above) and of nano-TiC observed in laboratory.  The 21 mm feature (the peak position is actually at 20.1 mm) has been duplicated by nano-TiC, but still disputable.  (Reference: von Helden, et alScience, 288 (2000) 313)

Why microgravity experiments using overseas rockets?

We are planning to use sounding rockets in US and Sweden together with Dr. Joseph A. Nuth III of NASA Goddard Space Flight Center and Prof. Jürgen Blum of Institute for geophysics and extraterrestrial physics.  Following is the reason why we need international collaborations.

Why microgravity experiment is required?  The reasons are Homogeneity of nucleation environment, slower cooling rate, monodispersivity of products and longer duration for infrared spectroscopy.

Why we use sounding rockets?  The reasons is to wait suppression of turbulence of buffer Ar gas and homogenize the temperature of an evaporation source.  In addition, several tens sec are required to measure the signal changes of infrared spectra due to crystallization. To suppress a convection current generated by an evaporation source, gravity condition less than 0.01% (10-4 G) is necessary.

Why overseas rocket is necessary?  Recovery of the sample allows us to determine size, number density, crystalline structure and crystallinity.

JSPS, Grant-in-Aid for Scientific Research(S):Nucleation

Term of Project:FY2015-2019

PI: Yuki Kimura (Hokkaido University)


The early stages of crystallization, called “nucleation” is an essential process because of beginning of material formation and importance in various fields.  I believe significant properties of nano-materials and hydrated layer on a material play a critical rule.  In this project, we tackle nucleation by in-situ observation using originally developed transmission electron microscopy and multi wavelength laser interferometry.  Physical and chemical mechanisms in the nucleation processes will be elucidated including a behavior of precursors.

Purpose and Background of the Research

Since “nucleation” is a fundamental process to form a material from atoms or molecules and has been believed to be determined characters of the products, understanding of the mechanism of nucleation is essential for material science. However, the detail of the process is still unknown since the modelling by Gibbs (1876). Recent years, new nucleation models have been proposed and actively debated.

In this project, we will perform in-situ transmission electron microscope (TEM) observation using a liquid cell and show the direct evidence of a relationship between nucleation and precursor. We believe that the keys to understand nucleation are characteristic properties of nanoparticles and hydrated layer. Therefore, physical properties (surface free energy and sticking probability) of nanoparticles will be determined by nucleation experiment from a vapor phase and the results of nucleation in water solution and in ionic liquid solution will be compared to know how hydrated layer works during nucleation. As the result, a new model of nucleation will be constructed.

Research Methods

Recently, we succeeded to make a system to observe a phenomena and a reaction of nanoparticles in a water solution. This system is a most powerful for visualization of nucleation process, which will be progressed in meso-scale. Individual nanoparticles can be observed and analyzed its crystal structure by electron diffraction. In vapor phase experiments, physical properties of nanoparticles will be determined based on supersaturation at the nucleation, which determined by double wavelength Mach-Zehnder-type interferometer (Fig. 1). The results will be compared with that obtained by molecular dynamics simulation or global reaction route mapping. As the result, we will construct an advanced nucleation model.

Figure 1. (a) Nucleation chamber with highly sensitive double wavelength Mach–Zehnder- type interferometer and (b) a typical example of the interference fringe at the moments of nucleation. The deviation of the fringe is a result of changing in refractive index of only 10-5by nucleation.

Expected Research Achievements and Scientific Significance

Current view of nucleation based on microscale phenomena by optical microscope will be nanoscale view by TEM. Our results will be contribute to the field of biomineralization and formation of biomaterial in near future.

  • Hokkaido University
  • Institute of Low Temperature Science. Hokkaido Univ