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🔥 Content Introduction
This MATLAB code repository focuses on the new technological feature (Technosignature) of “microthermal residuals generated by the interaction of directed electromagnetic radiation with the interstellar medium (ISM).” It quantifies beam divergence, temperature changes, and detectability through numerical simulation, providing new theoretical and experimental tools for the search for extraterrestrial intelligence (SETI). This article will systematically break down the code structure, simulation logic, and key reproduction points, while interpreting the scientific significance of the results in the context of astrophysics, aiding researchers in quickly getting started and expanding applications.
1. Core Background and Scientific Objectives of the Code Repository
In the field of SETI, traditional technological features (such as radio signals and laser pulses) face challenges of “signal interference and high background noise.” However, the microthermal residuals of directed electromagnetic radiation—specifically, the localized temperature increase left behind after narrow-beam electromagnetic radiation (such as communication or energy transmission beams from extraterrestrial civilizations) interacts with the interstellar medium—have unique advantages of “long duration and low background interference,” making it a potential technological feature proposed in 2025.
The core scientific objectives of the code repository are:
- Quantify the effects of different beam parameters (divergence angle, power, duration) and interstellar medium properties (density, temperature, composition) on thermal residuals;
- Evaluate the detectability of thermal residuals against cosmic background noise and determine observation thresholds;
- Provide observational parameter recommendations for ground/space telescopes (such as the James Webb Space Telescope JWST and the Square Kilometre Array SKA).
⛳️ Simulation Results
📣 Sample Code
🔗 References
“Microthermal Residuals from Directed Electromagnetic Emissions as a New Class of Technosignature” by Sergio Bonaque-González (2025), submitted for publication in April 2025
% Beam divergence after passing near a star, with reference divergence lines
clear; clc; close all % Clear environment and prepare workspace
% Physical constants
G = 6.6743e-11; % [m^3/kg/s^2]
M = 0.35*1.989e30; % solar mass [kg]
c = 2.99792458e8; % [m/s]
AU = 1.496e11; % [m]
R_sun = 6.96e8; % [m]
%% Simulation parameters:
b_vals = linspace(1, 5, 5) * R_sun; % Impact parameters: multiples of the solar radius
L_pc = linspace(1, 30000, 2000); % X axis: distance in [pc]
L_m = L_pc * 3.086e16; % [m]
theta_vals = [1e-7, 1e-8, 1e-9, 1e-10]; % Fixed beam divergences [rad]
baseline_theta = 1e-7; % for comparison purposes [rad]
regions = [153, 307, 1534, 30000];
%% Simulation
% Initialization
W = NaN(length(b_vals), length(L_m)); % NaN to hide pre-focus zone
% CASE 1: Calculates the post-focal beam envelope for rays grazing a lensing star
% at various impact parameters (b = 1? R_sun). Each ray experiences a
% deflection Theta = 4GM/(c^2), resulting in a focal distance f = b/Theta.
% Beyond the focal region, the beam expands linearly with Theta
🎈 Some theoretical references are from online literature; please contact the author for removal if there are any copyright issues.
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