(SG1) Multi-phase and Atomic/Molecular physics group report
June 4, 2024 (M. Kobayashi)
Date: May 31, 2024
Time: 15:35 -16:45
Shot#: 192477 – 192499 (23 shots)
Prior wall conditioning: No
Divertor pump: On
Gas puff: H2, N2 IPD: No
LID: No
NBI#(1, 2, 3, 4, 5)=gas(-, -, -, -, -)=P(-, -, -, -, -) MW
ECH(77GHz)=ant(5.5-U, 2-OUR)=P(698, 380)kW
ECH(154GHz)=ant(2-OLL, 2-OUL, 2O-LR)=P(705, 889, 982) kW
ECH(116GHz)=ant(2O-LR)=P(-)kW
ECH(56GHz)=ant(1.5-U)=P(-)kWICH(3.5U, 3.5L, 4.5U, 4.5L) = P(-, -, -, -) MW
Topics
1. Understanding of the evolution of cosmic organic dust in reaction with plasma (I. Sakon)

120240531

Understanding of the evolution of cosmic organic dust in reaction with plasma(I. Sakon, T. Miyata, T. Onaka, K. Kobayashi, Y. Kebukawa, J. Takahashi, M. Tanaka, H. Nakamura, M. Shoji, S. Masuzaki, M. Kobayashi)
Background & objectives: In the previous run (Cycle 24 experiment), the experiment was conducted at the LHD of the NIFS, irradiating hydrocarbon dust with a relatively lowenergy plasma (hydrogen and nitrogen) at the outer edge of the LHD plasma. Preliminary analysis revealed changes in infrared properties of filmy QCC that reproduce thecharacteristics of peculiar unidentified infrared bands observed in galaxies with weak active galactic nuclei (Smith et al. 2007) and in elliptical galaxies (Bregman et al. 2008;
Kaneda et al. 2005), characterized by the absence of the 6-9μm bands corresponding to stretching modes of aromatic C-C bonds and the presence of only the 11-14μm bandscorresponding to out-of-plane bending modes of aromatic C-H bonds. While the polycyclic aromatic hydrocarbons (PAHs) hypothesis is widely accepted in astronomy as thecarrier of these bands, the exact understanding of their nature is incomplete. Thus, the identification of the carrier responsible for these bands and the determination of thephysical factors giving rise to their characteristics remain unresolved for galaxies with weak active galactic nuclei and elliptical galaxies. Here we propose exposure experiment ofhydrocarbon solids to the Large helical Device (LHD) plasma by means of a movable sample holder in the 10.5-L port and collect organic dust on the Si or SiO2 substrate.The
present study aims to understand the properties of interstellar organic matter in space, based on an integrated approach involving astronomical observations, experimental
astrophysics, and molecular dynamics simulations.
Reference:[1] J. D. Bregman et al. 2008, ASP Conf. Ser. 381, 34, [2] I. Endo, I. Sakon, T. Onaka et al. 2021, ApJ, 917, 103, [3] H. Kaneda et al. 2005, ApJ, 632, 83, [4] J. D. T. Smith et al. 2007, ApJ, 656, 770

Results: 10mg of Coronene C24H12 on a SiO2 substrate (x1), a few mg of filmy QCC on a Si substrate(x2), a few mg of QNCC on Si substrate (x2) and a blank Si substrate (x1) are exposed to the Hydrogenand nitrogen plasma (low-energy part of the LHD plasma). N2 are supplied at 3.5L, 5.5L and 9.5L port.
Experiment parameters of each shot are given in the following table. The probe attached to the holder
confirmed that reaction with plasma flow of >1x1021 ions/s/m2 (TBR) was achieved for each shot.
Shot
ID

N2(3.5L)

N2(5.5L)

N2(9.5L)

comment

Shot
ID

N2(3.5L)

N2(5.5L)

N2(9.5L)

comment

192479200ms

1500ms

1500ms-300mm, collapse

192490

None

800ms

800ms-50mm, collapse

192480None

None

None-300mm

192491

None

None

None-50mm

192481150ms

1500ms

1500ms-300mm, collapse

192492

None

700ms

700ms

-30mm, OK

192482None

None

None-300mm

192493

None

700ms

700ms-30mm, OK

192483100ms

1500ms

1500ms-300mm, collapse

192494

None

700ms

700ms-10mm, OK

192484None

None

None-300mm

192495

None

700ms

700ms-20mm, collapse

192485None

1500ms

1500ms-300mm, collapse

192496None

None

None-25mm

192486None

None

None-300mm

192497

None

700ms

700ms

192487

None

800ms

800ms-300mm, OK-25mm, collapse,
no ECH

192488

None

800ms

800ms-100mm, collapse

192498None

None

None-25mm

192499

None

700ms

700ms-25mm, OK

192489None

None

None-100mm2

Experiment on LHD (cycle 25)
at National Institute for Fusion Science
QNCC#1 on Si substrate
Filmy QCC #1 on Si substrate (retrial of 20240510 experiment)C24H12 on SiO2 substrate(retrial of 20240510 experiment)

blank Si substrate
Filmy QCC #2 on Si substrate(retrial of 20240510 experiment)
QNCC#2 on Si substrate