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Interstellar Probe - where is the “nose” of the heliosphere?

Ratkiewicz Romana, Baraniecka Anna

Artificial Satellites : Journal of Planetary Geodesy

2023

Vol. 58, No. 1

14--28

In this paper are reviewed publications that were concerned about the discovery of the location of the heliopause “nose” by the Newtonian Approximation method and publications using the full three-dimensional magnetohydrodynamic simulations of the heliosphere that confirmed that discovery. Since we do not have a clear answer to the question of what the heliosphere looks like, in connection with the planned launch of the Interstellar Probe within this decade, there was a problem with deciding which direction to send it. The discovery of the movement of the “nose” of the heliopause depending on the direction of the interstellar magnetic field and the determination of the position of the “nose” is very important for this decision. Therefore, the purpose of the article is to answer the question of where is the “nose” of the heliopause. In the second part of the article, the possibility of changing the paradigm of scientific research projects related to interstellar missions (including those focused on the study of the heliosphere), among other things, by increasing the interdisciplinarity of research, is explored. As part of initiating such cooperation, the article develops social sciences themes related to the sustainable logistics of Interstellar Probe missions to increase public involvement in these projects.

Does the interstellar bow shock exist around the heliosphere?

Ratkiewicz R., Kotlarz J.

Prace Instytutu Lotnictwa

2016

Nr 4 (245)

178--188

The paper discusses results of global modeling of the heliosphere regarding the existence of the interstellar bow shock (BS) in front of the heliosphere. The Local Interstellar Medium (LISM) velocity vector (VIS) and temperature (TIS) originally determined through the velocity and temperature of the interstellar helium (He) flowing in the inner heliosphere and measured by the GAS instrument on Ulysses, recently have been challenged by new measurements of the He flow by the Interstellar Boundary Explorer (IBEX). These measurements have initiated discussions on the existence of the BS. The purpose of this paper is a brief overview of studies focusing on in situ measurements of the He flow by the instruments on Ulysses and IBEX missions and indication of the reasons for discrepancies created in the past few years and associated with the existence of the BS.

W pracy przedyskutowano wyniki globalnego modelowania heliosfery dotyczące istnienia czołowej fali uderzeniowej (BS) przed heliosferą. Wektor prędkości (VIS) i temperatura (TIS) lokalnej materii międzygwiazdowej (LISM) oryginalnie wyznaczone przez prędkość i temperaturę międzygwiazdowego helu (He) wpływającego do heliosfery i mierzonego przez przyrząd GAS na sondzie Ulysses, ostatnio zostały zakwestionowane przez nowe pomiary przepływu He wykonane przez sondę Interstellar Boundary Explorer (IBEX). Pomiary te zainicjowały dyskusję na temat istnienia BS. Celem niniejszego artykułu jest krótki przegląd badań poświęconych pomiarom in situ strumienia helu przez instrumenty na sondach Ulysses i IBEX oraz wskazanie przyczyn rozbieżności związanych z istnieniem czołowej fali uderzeniowej powstałych wciągu kilku ostatnich lat [51].