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Interstellar Probe — Where is the “Nose” of the Heliosphere?

Romana Ratkiewicz
Romana Ratkiewicz
 e 
Anna Baraniecka
Anna Baraniecka
   | 15 apr 2023
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Pubblicato online: 15 apr 2023
Pagine: 14 - 28
Ricevuto: 30 nov 2022
Accettato: 01 mar 2023
DOI: https://doi.org/10.2478/arsa-2023-0002
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© 2023 Romana Ratkiewicz et al., published by Sciendo
This work is licensed under the Creative Commons Attribution 4.0 International License.

Figure 1.

Different heliosphere shapes from numerical results: Comet-like Heliosphere, the Heliotail, Croissant, Bubble, Croissant and Bubble, and three-dimensional map of the heliosphere from IBEX
Different heliosphere shapes from numerical results: Comet-like Heliosphere, the Heliotail, Croissant, Bubble, Croissant and Bubble, and three-dimensional map of the heliosphere from IBEX

Figure 2.

The “nose” of the HP
The “nose” of the HP

Figure 3.

Dependence of the angular deviations θs of the HP “nose” for different inclination angles θo and different Alfvén Mach numbers (Ma) (Fahr et al., 1986, 1988)
Dependence of the angular deviations θs of the HP “nose” for different inclination angles θo and different Alfvén Mach numbers (Ma) (Fahr et al., 1986, 1988)

Figure 4.

Shape of the HP in the plane Bis-Vis that contains the LISM velocity and magnetic field vectors for different inclination angles Ψo (Fahr et al., 1986, 1988)
Shape of the HP in the plane Bis-Vis that contains the LISM velocity and magnetic field vectors for different inclination angles Ψo (Fahr et al., 1986, 1988)

Figure 5.

Shape of the boundary region as shown by thermal pressure contour plots for inclination angle α equal to a. 0°, b. 30°, c. 60°, d. 90°. VLISM Alfvén Mach number=1.5. Position of termination shock (TS), HP, and bow shock (BS) is indicated in the left panel (Ratkiewicz et al., 1998).
Shape of the boundary region as shown by thermal pressure contour plots for inclination angle α equal to a. 0°, b. 30°, c. 60°, d. 90°. VLISM Alfvén Mach number=1.5. Position of termination shock (TS), HP, and bow shock (BS) is indicated in the left panel (Ratkiewicz et al., 1998).

Figure 6.

Magnetic field pressure for ISMF inclination angle α equal to a. 0°, b. 67°, c. 90°. The ISMF pressure reaches its maximum (red) in the quasi-perpendicular direction to the unperturbed LISM magnetic field direction (Ratkiewicz et al., 2000).
Magnetic field pressure for ISMF inclination angle α equal to a. 0°, b. 67°, c. 90°. The ISMF pressure reaches its maximum (red) in the quasi-perpendicular direction to the unperturbed LISM magnetic field direction (Ratkiewicz et al., 2000).

Figure 7.

Thermal isobars in three coordinate planes, x-y, x-z, y-z, for inclination angles 0°, 67°, 90° show axisymmetric heliosphere (column A: parallel interstellar velocity and interstellar magnetic field vectors) and asymmetric heliosphere (column B: deviation in x-y plane, flattening in x-z and y-z planes for perpendicular ISMF and (column C: deviation in x-y plane, flattening in x-z plane, and distortion in y-z for oblique ISMF) (Ratkiewicz et al., 2000).
Thermal isobars in three coordinate planes, x-y, x-z, y-z, for inclination angles 0°, 67°, 90° show axisymmetric heliosphere (column A: parallel interstellar velocity and interstellar magnetic field vectors) and asymmetric heliosphere (column B: deviation in x-y plane, flattening in x-z and y-z planes for perpendicular ISMF and (column C: deviation in x-y plane, flattening in x-z plane, and distortion in y-z for oblique ISMF) (Ratkiewicz et al., 2000).

Figure 8.

Perfect confirmation of the deviation of the HP “nose” applies both to the heliosphere model without IMF (left panels) and with IMF (right panels) (courtesy Izmodenov and Alexashov, 2015).
Perfect confirmation of the deviation of the HP “nose” applies both to the heliosphere model without IMF (left panels) and with IMF (right panels) (courtesy Izmodenov and Alexashov, 2015).

Figure 9.

The created “tongue” is set towards the maximal ISMF on each line at right angles (blue circles) (courtesy Zirnstein et al., 2016).
The created “tongue” is set towards the maximal ISMF on each line at right angles (blue circles) (courtesy Zirnstein et al., 2016).

Paradigm shift in interstellar research projects (missions)

Elements of the paradigm The “old paradigm” of heliospheric research missions Anomalies and other factors influencing the paradigm shift The “new” paradigm of heliospheric research missions
The heliosphere modeling approach

Traditional

Based on theoretical data

Scientific discussion on current models of the heliosphere

Voyager probes reaching heliospheric boundary and real data availability

The development of artificial intelligence

Modern

Based on theoretical and empirical data Building or verification and testing of models as part of space missions and using modern technologies, such as artificial intelligence
Interstellar mission priorities

Designing space probe missions to ensure the greatest possible number of measurements and data

Single missions for which individual support systems are built (logistics, engineering, research, and management team)

Serious social and environmental problems on Earth (pandemic, climate crisis, social crisis, social inequalities)

Growing ecological awareness of the society and social pressure for sustainable development

Criticism of high spending on research projects by the public, decision-makers as well as among scientists

Sustainable interstellar missions with mainly scientific goals, but also environmental, social, and economic goals

Campaign missions that use available mission management systems, including logistics systems
Character and composition of research teams The research teams are mainly composed of scientists in the fields of physics, astrophysics, and astronomy, as well as engineers

The growing interest of scientists from other fields in space exploration

Increasing complexity of space missions

Pressure on the effectiveness of research projects

Research teams are interdisciplinary

They are composed of scientists from various fields who support the mission and benefit from its effects, integrating heliosphere research into the achievements of their fields
Communication of research projects with society/social involvement

Communication of research projects with the social environment reduced to short media information or information provided by government agencies (such as National Aeronautics and Space Administration) on their websites

Little public transparency of research projects

No social involvement

Development of communication technologies

The overabundance of data and information available on the web, making it difficult for the public to focus on research projects related to interstellar missions

The very long duration of interstellar missions and their high cost and risk

Intensive promotional activities for space projects within the three bodies (Earth, Moon, Mars) and focusing on social attention in this area

Creating information and image campaigns and broad promotion of research projects Including social and environmental goals in research projects

Building intellectual capital for future missions

High transparency of research projects and open access to data

High social involvement
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