The Experts below are selected from a list of 303 Experts worldwide ranked by ideXlab platform
H. Kanno - One of the best experts on this subject based on the ideXlab platform.
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Non-existence of the Linear Relation between TH (homogeneous nucleation temperature) and Tm (melting temperature) for aqueous H2SO4 solution
Chemical Physics Letters, 2011Co-Authors: M. Takehana, C. Viriyarattanasak, Kazuhito Kajiwara, H. KannoAbstract:Abstract Test of the Linear Relation between TH (homogeneous ice nucleation temperature) and Tm (melting temperature) was carried out for aqueous HCl and H2SO4 solutions. It is shown that the Linear Relation does not hold for aqueous H2SO4 solution. Enhancement of the ionization of sulfuric acid with decreasing temperature is the most likely cause for the curved Relation between TH and Tm. In addition, close examination of the TH and Tm data for aqueous HCl solution indicates that the TH versus Tm Relation for aqueous HCl solution seems very weakly curved.
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Linear Relation between TH (homogeneous ice nucleation temperature) and Tm (melting temperature) for aqueous solutions of sucrose, trehalose, and maltose
Chemical Physics Letters, 2007Co-Authors: H. Kanno, Makoto Soga, Kazuhito KajiwaraAbstract:Abstract Homogeneous ice nucleation temperatures ( T H s) of aqueous sucrose, trehalose, and maltose solutions were measured together with melting temperatures ( T m s). It is shown that there is a Linear Relation between T H and T m for these solutions. Almost identical supercooling behavior is observed for these aqueous disaccharide solutions.
Youhua Chu - One of the best experts on this subject based on the ideXlab platform.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
The Astrophysical Journal, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R{sub b} Almost-Equal-To 1.22 M/M{sub Sun} - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 M{sub Sun} will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring the properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
arXiv: Astrophysics of Galaxies, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R_b \approx 1.22M/Msun - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 Msun will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
Kazuhito Kajiwara - One of the best experts on this subject based on the ideXlab platform.
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Non-existence of the Linear Relation between TH (homogeneous nucleation temperature) and Tm (melting temperature) for aqueous H2SO4 solution
Chemical Physics Letters, 2011Co-Authors: M. Takehana, C. Viriyarattanasak, Kazuhito Kajiwara, H. KannoAbstract:Abstract Test of the Linear Relation between TH (homogeneous ice nucleation temperature) and Tm (melting temperature) was carried out for aqueous HCl and H2SO4 solutions. It is shown that the Linear Relation does not hold for aqueous H2SO4 solution. Enhancement of the ionization of sulfuric acid with decreasing temperature is the most likely cause for the curved Relation between TH and Tm. In addition, close examination of the TH and Tm data for aqueous HCl solution indicates that the TH versus Tm Relation for aqueous HCl solution seems very weakly curved.
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Linear Relation between TH (homogeneous ice nucleation temperature) and Tm (melting temperature) for aqueous solutions of sucrose, trehalose, and maltose
Chemical Physics Letters, 2007Co-Authors: H. Kanno, Makoto Soga, Kazuhito KajiwaraAbstract:Abstract Homogeneous ice nucleation temperatures ( T H s) of aqueous sucrose, trehalose, and maltose solutions were measured together with melting temperatures ( T m s). It is shown that there is a Linear Relation between T H and T m for these solutions. Almost identical supercooling behavior is observed for these aqueous disaccharide solutions.
Ping Zhou - One of the best experts on this subject based on the ideXlab platform.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
The Astrophysical Journal, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R{sub b} Almost-Equal-To 1.22 M/M{sub Sun} - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 M{sub Sun} will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring the properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
arXiv: Astrophysics of Galaxies, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R_b \approx 1.22M/Msun - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 Msun will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
Yang Chen - One of the best experts on this subject based on the ideXlab platform.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
The Astrophysical Journal, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R{sub b} Almost-Equal-To 1.22 M/M{sub Sun} - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 M{sub Sun} will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring the properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
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Linear Relation for wind blown bubble sizes of main sequence ob stars in a molecular environment and implication for supernova progenitors
arXiv: Astrophysics of Galaxies, 2013Co-Authors: Yang Chen, Ping Zhou, Youhua ChuAbstract:We find a Linear Relationship between the size of a massive star's main-sequence bubble in a molecular environment and the star's initial mass: R_b \approx 1.22M/Msun - 9.16 pc, assuming a constant interclump pressure. Since stars in the mass range of 8 to 25-30 Msun will end their evolution in the red supergiant phase without launching a Wolf-Rayet wind, the main-sequence wind-blown bubbles are mainly responsible for the extent of molecular gas cavities, while the effect of the photoionization is comparatively small. This Linear Relation can thus be used to infer the masses of the massive star progenitors of supernova remnants (SNRs) that are discovered to evolve in molecular cavities, while few other means are available for inferring properties of SNR progenitors. We have used this method to estimate the initial masses of the progenitors of eight SNRs: Kes 69, Kes 75, Kes 78, 3C 396, 3C 397, HC 40, Vela, and RX J1713-3946.
