text: 259,34,1341615441697894400,1185977761032110080,Kazumasa Ohno (大野 和正),"A new paper posted! Though the paper is still under review, we have studied haze formation on Triton, an ultra-cold moon of Neptune, using microphysical models. We have discussed what physical processes are going on in Triton's cold and hazy atmosphere. <LINK> We developed a bin-scheme microphysical model that can trace size and porosity distributions of haze particles in a self-consistent manner. We tested several possible nature of Triton hazes, namely Titan-like sphere and aggregate haze, as well as the hazes coated by C2H4 ices. In a nutshell, our main conclusion is that condensation of C2H4 ices likely play crucial role to control physical and optical properties of Triton hazes. It is hard to explain existing observations of Triton hazes by Voyager 2 assuming Titan-like haze without condensation. Both sphere and aggregate icy hazes can reasonably explain observations, so it is currently difficult to conclude which is true. As the spectral behavior and scattering properties are different, future mission on outer solar system will help to unveil the morphological nature. In both sphere and aggregate cases, total haze mass flux (tholin+ice) is about an order of magnitude lower than that on Triton. Given predominant icy composition, Titan-like haze production rate on Triton is likely much lower than that on Titan. Our findings are bloadly consistent with the results and expectation of a Pluto (+Triton) haze paper that appeared in recent Nature Astronomy. I hope our works can complement their paper. <LINK> The paper is my first solar system paper. The results highlight a deep connection between haze and cloud formation: vapor condensation considerably alter the haze properties, depending on thermal structure. Hopefully, I would like to explore this phenomena in exoplanet context.",https://arxiv.org/abs/2012.11932,"The largest moon of Neptune, Triton, possess a cold and hazy atmosphere. Since the discovery of near-surface haze layer during the Voyager fly in 1989, the haze formation mechanism has not been investigated in detail. Here, we provide the first haze microphysical model on Triton. Our model solves the evolution of both size and porosity distributions of haze particles in a self-consistent manner. We simulated the formation of sphere and aggregate hazes with and without condensation of the C$_2$H$_4$ ice. The haze particles can grow into fractal aggregates with mass-equivalent sphere sizes of $\sim0.1$--$1~{\rm {\mu}m}$ and fractal dimension of $D_{\rm f} = 1.8$--$2.2$. The ice-free hazes cannot simultaneously explain both UV and visible observations of Voyager 2, while including the condensation of C$_2$H$_4$ ices provides two better solutions. For ice aggregates, the required total haze mass flux is $\sim2\times{10}^{-15}~{\rm g~{cm}^{-2}~s^{-1}}$. For the icy sphere scenario, the column integrated C$_2$H$_4$ production rate is $\sim8\times{10}^{-15}~{\rm g~{cm}^{-2}~s^{-1}}$, and the ice-free mass flux of $\sim6\times{10}^{-17}~{\rm g~{cm}^{-2}~s^{-1}}$. The UV occultation observations at short wavelength $<0.15~{\rm {\mu}m}$ may slightly favor the icy aggregates. Observations of the haze optical depth and the degree of forward scattering in UV and visible should be able to distinguish whether Triton's hazes are icy spheres or ice aggregates in future Triton missions. ",Haze Formation on Triton,7,"[""A new paper posted! Though the paper is still under review, we have studied haze formation on Triton, an ultra-cold moon of Neptune, using microphysical models. We have discussed what physical processes are going on in Triton's cold and hazy atmosphere.\n<LINK>"", 'We developed a bin-scheme microphysical model that can trace size and porosity distributions of haze particles in a self-consistent manner. We tested several possible nature of Triton hazes, namely Titan-like sphere and aggregate haze, as well as the hazes coated by C2H4 ices.', 'In a nutshell, our main conclusion is that condensation of C2H4 ices likely play crucial role to control physical and optical properties of Triton hazes. It is hard to explain existing observations of Triton hazes by Voyager 2 assuming Titan-like haze without condensation.', 'Both sphere and aggregate icy hazes can reasonably explain observations, so it is currently difficult to conclude which is true. As the spectral behavior and scattering properties are different, future mission on outer solar system will help to unveil the morphological nature.', 'In both sphere and aggregate cases, total haze mass flux (tholin+ice) is about an order of magnitude lower than that on Triton. Given predominant icy composition, Titan-like haze production rate on Triton is likely much lower than that on Titan.', 'Our findings are bloadly consistent with the results and expectation of a Pluto (+Triton) haze paper that appeared in recent Nature Astronomy. I hope our works can complement their paper.\nhttps://t.co/rQEbeARDv2', 'The paper is my first solar system paper. The results highlight a deep connection between haze and cloud formation: vapor condensation considerably alter the haze properties, depending on thermal structure. Hopefully, I would like to explore this phenomena in exoplanet context.']",20,12,1810