Meng Jin

Lockheed Martin (United States)

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W. B. Manchester

University of Michigan–Ann Arbor

B. van der Holst

University of Michigan–Ann Arbor

T. I. Gombosi

University of Michigan–Ann Arbor

ИВ

И. В. Соколов

University of Michigan–Ann Arbor

N. Nitta

Lockheed Martin (United States)

Mark C. M. Cheung

Hong Kong Polytechnic University

Vladimir Airapetian

Goddard Space Flight Center

Chuanfei Dong

Boston University

James Mason

Goddard Space Flight Center

G. Tóth

University of Michigan–Ann Arbor

Cooperative Institutions

Goddard Space Flight Center

178

Heliophysics

Centre National de la Recherche Scientifique

Max Planck Society

University of Colorado Boulder

University of Michigan–Ann Arbor

Laboratory for Atmospheric and Space Physics

Max Planck Institute for Solar System Research

University of California, Berkeley

Johns Hopkins University Applied Physics Laboratory

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Expanding The Frontiers: From The Solar Corona and The Wind to Evolving Space Weather of Planet Hosting Stars

Bulletin of the AAS (2023)

Vladimir Airapetian Meng Jin Junxiang Hu B. J. Lynch James Green

Whitepaper #005 in the Decadal Survey for Solar and Space Physics (Heliophysics) 2024-2033. Main topics: basic research. Additional topics: other basic research; ground-based missions/projects; solar physics; space-based missions/projects.

Space Weather

Corona (planetary geology)

10.3847/25c2cfeb.41e10693

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Citations (1)

High-accuracy mode recognition method in orbital angular momentum optical communication system

Chinese Optics Letters (2021)

Lin Zhao Yuan Hao Li Chen Wenyi Liu Meng Jin

Vortex optical communication has been a hot research field in recent years. A key step is mode recognition in the orbital angular momentum (OAM) free-space optical (FSO) communication system. In this article, we propose an OAM mode recognition method based on image recognition technology, which uses the interferogram between the vortex beam and the Gaussian beam to identify the OAM mode. In order to resist the influence of atmospheric turbulence on the recognition accuracy, we added a Gaussian smoothing filter into the recognition process. Moreover, we used random phase screens to generate interferogram sets at distances of 1 km and 2 km. The verification result shows that the proposed scheme produces high identification accuracy for the distorted optical field. The average accuracy can reach 100% and 87.78% under the conditions of medium- and strong-turbulence levels, respectively. It is anticipated that these results might be helpful for improving the reliability of the OAM-FSO communication system in the future.

Free-Space Optical Communication

Mode (computer interface)

Optical vortex

Gaussian filter

Gaussian beam

Smoothing

10.3788/col202220.020601

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Citations (14)

Incorporating observations in global models of the solar atmosphere

Solar Heliospheric and INterplanetary Environment (SHINE 2012) (2012)

W. B. Manchester Meng Jin B. van der Holst R. A. Frazin A. M. Vásquez

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On the importance of investigating CME complexity evolution during interplanetary propagation

Bulletin of the AAS (2023)

R. M. Winslow Noé Lugaz B. Schmieder Manuela Temmer C. J. Farrugia

This white paper brings to light the need for comprehensive studies on the evolution of interplanetary coronal mass ejection (ICME) complexity during propagation.To date, few studies of ICME complexity exist.In this white paper, we define ICME complexity and accompanying changes in complexity, describe recent works and their limitations, and outline key science questions that need to be tackled.In order to be able to address these science questions from a fundamental physics perspective, our main recommendations for the Decadal Survey Committee for Solar & Space Physics (Heliophysics) 2024-2033 are:• Prioritize spacecraft missions that can obtain comprehensive in situ ICME measurements at multiple heliocentric distances in the inner heliosphere.• Explore options, through simulations, for optimal spacecraft configuration in terms of radial, longitudinal, and latitudinal spacing to achieve the necessary spatial resolution to fully investigate ICME complexity evolution.• Once the data are available, focus efforts on comprehensive/holistic studies of ICME complexity evolution, integrating the results from many vantage points.Fundamental research on ICME complexity changes from the solar corona to 1 AU and beyond is critical to our physical understanding of the evolution and interaction of transients in the inner heliosphere.Furthermore, a complete understanding of such changes is required to understand the space weather impact of ICMEs at different planets.

10.3847/25c2cfeb.605c3041

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Solar Wind Model in the SWMF

И. В. Соколов Richard E. Mullinex A. Taktakishvili Doga Can Su Ozturk Judit Szente

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Characteristics of the 2017 September 10 GLE event in relation to shock properties

AGU Fall Meeting Abstracts (2019)

Bei Zhu Yuyang Liu Ryun-Young Kwon Meng Jin Zhirong Yang

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a Numerical Study of Long-Range Magnetic Impacts during Coronal Mass Ejections

shin (2016)

Meng Jin C. J. Schrijver Mark C. M. Cheung Marc L. DeRosa N. Nitta

Nanoflares

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The solar wind from a stellar perspective: how do low-resolution data impact the determination of wind properties?

arXiv (Cornell University) (2020)

S. Boro Saikia Meng Jin C. P. Johnstone T. Lüftinger M. Güdel

Alfv\'en-wave-driven 3D magnetohydrodynamic (MHD) models, which are increasingly used to predict stellar wind properties, contain unconstrained parameters and rely on low-resolution stellar magnetograms. We explore the effects of the input Alfv\'en wave energy flux and the surface magnetogram on the wind properties predicted by the Alfv\'en Wave Solar Model (AWSoM). We lowered the resolution of two solar magnetograms during solar cycle maximum and minimum using spherical harmonic decomposition. The Alfv\'en wave energy was altered based on non-thermal velocities determined from a far ultraviolet (FUV) spectrum of the solar twin 18 Sco. Additionally, low-resolution magnetograms of three solar analogues were obtained using Zeeman Doppler imaging (ZDI). Finally, the simulated wind properties were compared to Advanced Composition Explorer (ACE) observations. AWSoM simulations using well constrained input parameters taken from solar observations can reproduce the observed solar wind mass and angular momentum loss rates. The resolution of the magnetogram has a small impact on the wind properties and only during cycle maximum. However, variation in Alfv\'en wave energy influences the wind properties irrespective of the solar cycle activity level. Furthermore, solar wind simulations carried out using the low-resolution magnetogram of the three stars instead of the solar magnetogram could lead to an order of a magnitude difference in the simulated wind properties. The choice in Alfv\'en energy has a stronger influence on the wind output compared to the magnetogram resolution. The influence could be even stronger for stars whose input boundary conditions are not as well constrained as those of the Sun. Unsurprisingly, replacing the solar magnetogram with a stellar magnetogram could lead to completely inaccurate solar wind properties, and should be avoided in solar and stellar wind simulations.

Magnetogram

Corona (planetary geology)

Solar minimum

Solar observatory

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Learn to Walk Before You Run: A Case for Fundamental CME Research Utilizing Idealized MHD Models

Bulletin of the AAS (2023)

Tibor Török Noé Lugaz Christina O. Lee Erika Palmerio B. J. Lynch

Coronal mass ejections (CMEs) are the largest energy release events in the solar system (together with flares), and an integral part of the dynamics of the Sun's corona and the inner heliosphere.Despite a plethora of unsolved science questions regarding these enigmatic events, it appears that focus has been gradually shifting in recent years from fundamental CME research (and its encouragement via solicitations) towards research that is predominantly driven by understanding and predicting space weather.For the CME numerical modeling community in particular, it has become increasingly important to evolve towards developing practical applications, such as community models or operational space-weather forecasting tools ("Research to Operations").While we support the latter trend, we strongly caution against simultaneously neglecting fundamental CME research (and the utilization of simple, idealized MHD simulations), driven by the disputable perception that our knowledge of CMEs has sufficiently evolved to finally put it to 'practical use'.In this paper, we discuss the current situation and illustrate the enduring importance of fundamental CME research, and the usefulness of idealized models, based on selected unsolved science questions.To counteract the looming further decrease of fundamental CME research in our community, we recommend to (1) generally encourage and support fundamental research and 'simple' modeling approaches; (2) establish a new, focused funding opportunity for such research in the field of heliophysics; and (3) foster synergy on fundamental CME research between the solar and the plasma physics and stellar communities.

10.3847/25c2cfeb.395f28b4

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Atmospheric Escape From TOI-700 d: Venus versus Earth Analogs

Chuanfei Dong Meng Jin Manasvi Lingam

The recent discovery of an Earth-sized planet (TOI-700 d) in the habitable zone of an early-type M-dwarf by the Transiting Exoplanet Survey Satellite constitutes an important advance. In this Letter, we assess the feasibility of this planet to retain an atmosphere -- one of the chief ingredients for surface habitability -- over long timescales by employing state-of-the-art magnetohydrodynamic models to simulate the stellar wind and the associated rates of atmospheric escape. We take two major factors into consideration, namely, the planetary atmospheric composition and magnetic field. In all cases, we determine that the atmospheric ion escape rates are potentially a few orders of magnitude higher than the inner Solar system planets, but TOI-700 d is nevertheless capable of retaining a $1$ bar atmosphere over gigayear timescales for certain regions of the parameter space. The simulations show that the unmagnetized TOI-700 d with a 1 bar Earth-like atmosphere could be stripped away rather quickly ($<$ 1 gigayear), while the unmagnetized TOI-700 d with a 1 bar CO$_2$-dominated atmosphere could persist for many billions of years; we find that the magnetized Earth-like case falls in between these two scenarios. We also discuss the prospects for detecting radio emission of the planet (thereby constraining its magnetic field) and discerning the presence of an atmosphere.

Atmospheric escape

Planetary habitability

Atmospheric models

Atmosphere of Venus

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