https://ogma.newcastle.edu.au/vital/access/ /manager/Index en-au 5 https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:37383 Wed 28 Oct 2020 11:05:03 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:17050 Wed 11 Apr 2018 15:36:30 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:17051 θ) is represented by a power-law function of Reynolds number, and it approaches 5/3 faster than that for the velocity spectrum (mu). Results show that the ratio between the velocity and temperature scaling range exponents, (5/3+m_u)/m_θ, is about 1.98.]]> Wed 11 Apr 2018 15:29:00 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:21717 Wed 11 Apr 2018 13:37:27 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:25562 Tue 25 Jul 2023 12:17:33 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:38094 ⊙ infrared dark molecular filament that exhibits large NH₃ velocity dispersions (σ ~ 8 km s⁻¹) and bright, narrow NH₃(3, 3) line emission. We have probed G23.33-0.30 at the < 0.1 pc scale and confirmed that the narrow NH₃(3, 3) line is emitted by four rare NH₃(3, 3) masers, which are excited by a large-scale shock impacting the filament. G23.33-0.30 also displays a velocity gradient along its length, a velocity discontinuity across its width, shock-tracing SiO(5–4) emission extended throughout the filament, and broad turbulent line widths in NH₃(1, 1) through (6, 6), CS(5–4), and SiO(5–4), as well as an increased NH₃ rotational temperature (T_rot) and velocity dispersion (σ) associated with the shocked, blueshifted component. The correlations among T_rot, σ, and V_LSR imply that the shock is accelerating, heating, and adding turbulent energy to the filament gas. Given G23.33-0.30's location within the giant molecular cloud G23.0-0.4, we speculate that the shock and NH₃(3, 3) masers originated from the supernova remnant (SNR) W41, which exhibits additional evidence of an interaction with G23.0-0.4. We have also detected the 1.3 mm dust continuum emission from at least three embedded molecular cores associated with G23.33-0.30. Although the cores have moderate gas masses (M = 7–10 M_⊙), their large virial parameters (α = 4–9) suggest that they will not collapse to form stars. The turbulent line widths of the (α > 1) cores may indicate negative feedback due to the SNR shock.]]> Tue 03 Aug 2021 18:28:28 AEST ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:20796 Sat 24 Mar 2018 08:05:59 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:21028 in situ scanning tunnelling microscopy (STM) has been employed to elucidate the structure of the charged Au(111)–ionic liquid (1-butyl-1-methylpyrrolidinium tris(pentafluoroethyl)trifluorophosphate, [Py_1,4]FAP) interface in the presence of 0.1 M LiCl. The addition of the Li salt to the ionic liquid has a strong influence on the interfacial structure. In the first STM scan in situ measurements reveal that Au(111) undergoes the (22 x √3) 'herringbone' reconstruction in a certain potential regime, and there is strong evidence that the gold surface dissolves at negative electrode potentials in [Py_1,4]FAP containing LiCl. Bulk deposition of Li is obtained at −2.9 V in the second STM scan.]]> Sat 24 Mar 2018 07:50:31 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:27366 Sat 24 Mar 2018 07:36:41 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:27343 Sat 24 Mar 2018 07:24:07 AEDT ]]> https://ogma.newcastle.edu.au/vital/access/ /manager/Repository/uon:40043 Fri 22 Jul 2022 13:20:28 AEST ]]>