Shoji Mori
A5077567267- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- Stellar, planetary, and galactic studies
- Molecular Spectroscopy and Structure
- Phase Equilibria and Thermodynamics
- Advanced Chemical Physics Studies
- Quantum, superfluid, helium dynamics
- Atmospheric Ozone and Climate
- 3D IC and TSV technologies
- Organ Transplantation Techniques and Outcomes
- Atomic and Subatomic Physics Research
- VLSI and Analog Circuit Testing
- Animal Nutrition and Physiology
- Low-power high-performance VLSI design
- VLSI and FPGA Design Techniques
- Insect and Pesticide Research
- Magnetic and Electromagnetic Effects
- Mitochondrial Function and Pathology
- Plasma Diagnostics and Applications
- Aquaculture Nutrition and Growth
- Silicon and Solar Cell Technologies
- Livestock and Poultry Management
- Solar and Space Plasma Dynamics
- Advanced Condensed Matter Physics
- Dust and Plasma Wave Phenomena
Tohoku University
2021-2024
The University of Tokyo
2019-2024
Tokyo Institute of Technology
2014-2022
Nagoya University
1984-2016
Graduate School USA
2015
Toshiba (Japan)
2002-2003
Advanced Science Research Center
1999-2000
University of Kochi
2000
Kōchi University
2000
Toshiba (South Korea)
1991
We present an overview of the Large Program, ``Early Planet Formation in Embedded Disks (eDisk)'', conducted with Atacama Millimeter/submillimeter Array (ALMA). The ubiquitous detections substructures, particularly rings and gaps, protoplanetary disks around T Tauri stars raise possibility that at least some planet formation may have already started during embedded stages star formation. In order to address exactly how when is initiated, program focuses on searching for substructures 12...
Abstract We present observations of the Class 0 protostar IRAS 16544–1604 in CB 68 from “Early Planet Formation Embedded Disks (eDisk)” ALMA Large program. The target continuum and lines at 1.3 mm with an angular resolution ∼5 au. image reveals a dusty protostellar disk radius ∼30 au seen close to edge-on asymmetric structures along both major minor axes. While asymmetry axis can be interpreted as effect dust flaring, comes real nonaxisymmetric structure. C 18 O cubes clearly show gas that...
Constraining the physical and chemical structure of young embedded disks is crucial to understanding earliest stages planet formation. As part Early Planet Formation in Embedded Disks Atacama Large Millimeter/submillimeter Array Program, we present high spatial resolution ($\sim$0$.\!\!^{\prime\prime}$1 or $\sim$15 au) observations 1.3 mm continuum $^{13}$CO $J=$ 2-1, C$^{18}$O SO $J_N=$ $6_5$-$5_4$ molecular lines toward disk around Class I protostar L1489 IRS. The emission shows a...
Abstract We performed radiative transfer calculations and observing simulations to reproduce the 1.3 mm dust-continuum C 18 O (2–1) images in Class I protostar R CrA IRS7B-a, observed with ALMA Large Program “Early Planet Formation Embedded Disks (eDisk).” found that a dust disk model passively heated by central cannot peak brightness temperature of continuum emission (∼195 K), regardless assumptions about opacity. Our calculation suggests viscous accretion heating is required high...
Abstract We have observed the Class 0/I protostellar system Ced110 IRS4 at an angular resolution of 0.″05 (∼10 au) as part Atacama Large Millimeter/submillimeter Array large program, Early Planet Formation in Embedded Disks. The 1.3 mm dust continuum emission reveals that is a binary with projected separation ∼250 au. emissions associated main source and its companion, named IRS4A IRS4B, respectively, exhibit disk-like shapes likely arise from disks around protostars. has radius ∼110 au...
The magnetorotational instability (MRI) drives vigorous turbulence in a region of protoplanetary disks where the ionization fraction is sufficiently high. It has recently been shown that electric field induced by MRI can heat up electrons and thereby affect balance gas. In particular, disk abundant dust grains are present, electron heating causes reduction abundance, preventing further growth MRI. By using nonlinear Ohm's law takes into account heating, we investigate this negative feedback...
ABSTRACT The study of hot corinos in solar-like protostars has been so far mostly limited to the Class 0 phase, hampering our understanding their origin and evolution. In addition, recent evidence suggests that planet formation starts already during I which therefore represents a crucial step future planetary system chemical composition. Hence, become paramount importance. Here, we report discovery corino towards prototypical protostar L1551 IRS5, obtained within ALMA (Atacama Large...
Abstract We have observed the very low-mass Class 0 protostar IRAS 15398−3359 at scales ranging from 50 to 1800 au, as part of Atacama Large Millimeter/Submillimeter Array Program FAUST. uncover a linear feature, visible in H 2 CO, SO, and C 18 O line emission, which extends source direction almost perpendicular known active outflow. Molecular emission SiO, CH 3 OH further reveals an arc-like structure connected outer end feature separated protostar, 15398−3359, by 1200 au. The is...
Abstract We have observed the late Class I protostellar source Elias 29 at a spatial resolution of 70 au with Atacama Large Millimeter/submillimeter Array as part FAUST Program. focus on line emission SO, while that 34 C 18 O, CS, SiO, H 13 CO + , and DCO are used supplementarily. The distribution SO rotational temperature ( T rot (SO)) is evaluated by using intensity ratio its two excitation lines. Besides in vicinity protostar, hot spots found distance 500 from protostar; (SO) locally...
Abstract We report a study of the low-mass Class 0 multiple system VLA 1623AB in Ophiuchus star-forming region, using H 13 CO + ( J = 3–2), CS 5–4), and CCH N 3–2) lines as part ALMA Large Program FAUST. The analysis velocity fields revealed rotation motion envelope gradients outflows (about 2000 au down to 50 au). further investigated circumbinary 1623A disk, well 1623B disk. found that minor axis disk is misaligned by about 12° with respect large-scale outflow envelope. In contrast,...
With widespread recent emphasis on System-On-a-Chip (SOC), IP reuse has emerged as a vital and growing business in semiconductor industry. In this paper, we will address essential issues for by discussing current challenges to the success of businesses identifying obstacles that need be overcome.
The gas temperature in protoplanetary disks (PPDs) is determined by a combination of irradiation heating and accretion heating, with the latter conventionally attributed to turbulent dissipation. However, recent studies have suggested that inner disk (a few AU) largely laminar, primarily driven magnetized winds, as result nonideal magnetohydrodynamic (MHD) effects from weakly ionized gas, suggesting an alternative mechanism Joule We perform local stratified MHD simulations including all...
Abstract The low water content of the terrestrial planets in solar system suggests that protoplanets formed within snow line. Accurate prediction line location moving with time provides a clue to constraining formation process planets. In this paper, we investigate migration protoplanetary disks whose accretion is controlled by laminar magnetic fields, which have been proposed various nonideal magnetohydrodynamic (MHD) simulations. We propose an empirical model disk temperature based on our...
Abstract The chemical diversity of low-mass protostellar sources has so far been recognized, and environmental effects are invoked as its origin. In this context, observations isolated without the influence nearby objects particular importance. Here, we report physical structures Class 0 source IRAS 16544−1604 in Bok globule CB 68, based on 1.3 mm Atacama Large Millimeter/submillimeter Array at a spatial resolution ∼70 au that were conducted part large program FAUST. Three interstellar...
Abstract Cylindrical molecular filaments are observed to be the main sites of Sunlike star formation, while massive stars form in dense hubs at junction multiple filaments. The role hub–filament configurations has not been discussed yet relation birth environment solar system and infer origin isotopic ratios short-lived radionuclides (SLR, such as 26 Al) calcium–aluminum-rich inclusions (CAIs) meteorites. In this work, we present simple analytical estimates impact stellar feedback on young...
The temperature structure of protoplanetary disks provides an important constraint on where in the rocky planets like our own form. Recent nonideal magnetohydrodynamical (MHD) simulations have shown that internal Joule heating associated with magnetically driven disk accretion is inefficient at midplane. A model based MHD predicts a around solar-mass young star, water snow line can move inside current Earth's orbit within 1 Myr after formation. However, efficiency depends disk's ionization...
Methanol is a ubiquitous species commonly found in the molecular interstellar medium. It also crucial seed for building-up of chemical complexity star forming regions. Thus, understanding how its abundance evolves during formation process and whether it enriches emerging planetary system paramount importance. We used new data from ALMA Large Program FAUST (Fifty AU STudy chemistry disk/envelope Solar-like protostars) to study methanol line emission towards [BHB2007] 11 protobinary (sources A...
Abstract A polarized absorption spectrum of biphenylene was measured at a low temperature using stretched polymer film technique. The polarizations the bands positioned 253 and 200 nm were determined to be long‐axis short‐axis polarized, respectively. mechanism is proposed in which intensity first symmetry forbidden band system induced merely by coupling with vibration b 2u skeletal deformation without borrowing from nearby band. vibrational analysis for second also examined views film.
We performed synthetic observations of the Ulrich, Cassen, and Moosman (UCM) model to understand relation between physical structures infalling envelope around a protostar their observational features in molecular lines, adopting L1527 as an example. also compared structure position-velocity (P-V) diagrams UCM simple ballistic (SB) model. There are multiple ways compare data with data. first calculated correlation coefficient. The SB show similarly good While reflects overall similarity cube...
H atoms produced by the γ-ray irradiation of solid para-H2 (p-H2) and normal-H2 (n-H2) decay gradually when irradiated sample is stored at 4.2 K. ortho-H2 (o-H2) molecules sites nearest an atom in n-H2 convert to p-H2 interacting with atom. H2 process tunneling diffusion + → finally recombine other atoms. The rate constants for reaction were obtained from rates various concentrations o-H2. When 10 h K after irradiation, a number o-H2 change into catalytic chain induced mobile G value yields...
ABSTRACT It has been considered that large satellites around gas planets form in situ circumplanetary discs (CPDs). However, dust particles supplied into CPDs drift toward the central before they grow satellitesimals, building blocks of satellites. We investigate growth laminar with magnetic wind-driven accretion. In such discs, can settle on to mid-plane and by mutual collision more efficient than classical turbulent CPDs. First, we carry out 3D local MHD simulations a CPD including all...
Abstract Magnetorotational instability (MRI) has the potential to generatevigorous turbulence in protoplanetary disks, although its strength and accretion stress remain debatable because of uncertainty MRI with a low ionization fraction. We focus on heating electrons by strong electric fields, which amplifies nonideal magnetohydrodynamic effects. The heated frequently collide stick dust grains, turn decreases fraction is expected weaken turbulent motion driven MRI. In order quantitatively...
A sharp singlet signal assigned to electron bubbles was observed in γ-irradiated solid para-H2−D2 (HD) mixtures by use of high-resolution ESR spectroscopy. The not pure para-H2 but the mixtures. This result indicates that D2 and HD molecules play an important role formation para-H2. decay with a half-lifetime about 2 h, rate constant at 4.2 K is very close 2.2 K. shows migrate p-H2 sample via quantum mechanical tunneling.