The Era of Multi-Messenger Solar Physics (IAU S372)

Multi-messenger science in solar astronomy has a long history, but the recent advent of major observational facilities is heralding an exciting new era of scientific opportunities. This volume collects the proceedings of IAU Symposium 372, focusing on how these facilities can address pressing questions in solar physics, with a special emphasis on coordinated operation and synergies.

Format: Hardback
Length: 200 pages
Publication date: 09 November 2023
Publisher: Cambridge University Press

Solar astronomy has a rich history in multi-messenger science, with direct measurements of "in-situ" particles originating from the Sun, such as the solar wind, being used alongside remote observations to shape our understanding of the heliosphere. However, the recent emergence of several significant observational facilities, including the Parker Solar Probe, Solar Orbiter, and the Inouye Solar Telescope, among many others, is ushering in an exciting new era of scientific opportunities in multi-messenger solar physics. This volume, which collects the proceedings of IAU Symposium 372 held during the XXXIst IAU General Assembly in Busan, Republic of Korea, aims to showcase how these facilities can address numerous pressing questions in contemporary solar physics, with a particular focus on their coordinated operation and the resulting synergies. Graduate students and researchers in solar physics will greatly benefit from the many new results presented within.

The study of particles that originate from the Sun and travel through space is known as solar astronomy. It involves observing and analyzing these particles to gain insights into the Sun's behavior and its impact on the surrounding solar system. Solar astronomy has a long history, dating back to the early 19th century when scientists began using telescopes to observe the Sun's surface and detect its emissions. Over time, advances in technology have allowed scientists to study these particles in greater detail and at different wavelengths of light.

One of the key tools used in solar astronomy is the solar wind, which is a stream of charged particles that flows outward from the Sun's surface. The solar wind is composed of protons, electrons, and other charged particles that are ejected from the Sun's corona, the outermost layer of its atmosphere. The speed of the solar wind can vary greatly, ranging from a few hundred kilometers per second to over 1,000 kilometers per second. The solar wind plays an important role in shaping the structure of the heliosphere, the vast region of space that surrounds the Sun and is influenced by its magnetic field.

Another important aspect of solar astronomy is the study of coronal mass ejections (CMEs), which are large eruptions of plasma that occur on the Sun's surface. CMEs are responsible for many of the phenomena that occur in the solar system, such as solar flares, coronal holes, and geomagnetic storms. Scientists use a variety of instruments to observe and study CMEs, including spacecraft, ground-based telescopes, and space-based instruments such as the Solar Orbiter and the Parker Solar Probe.

In addition to studying the Sun's immediate environment, solar astronomy also involves studying the Sun's influence on other celestial bodies in the solar system. For example, scientists use solar wind measurements to study the behavior of comets and other icy bodies in the outer solar system, and they use observations of the Sun's corona to study the behavior of planets in the inner solar system.

One of the most exciting developments in solar astronomy in recent years has been the emergence of multi-messenger science. Multi-messenger science involves the study of particles that originate from the Sun and travel through space, as well as the study of gravitational waves and other electromagnetic radiation that are emitted by the Sun. By combining observations of these different types of radiation, scientists can gain a more comprehensive understanding of the Sun's behavior and its impact on the surrounding solar system.

One of the key facilities used in multi-messenger solar physics is the Solar Orbiter, which is a spacecraft that was launched by the European Space Agency in 2020. The Solar Orbiter is designed to study the Sun's corona in great detail, and it is equipped with a suite of instruments that measure the magnetic field system, the solar wind, and the corona's plasma. The Solar Orbiter is also equipped with a coronagraph, which is a device that allows scientists to study the Sun's corona in three dimensions, providing a more complete picture of the Sun's activity.

Another important facility used in multi-messenger solar physics is the Parker Solar Probe, which is a spacecraft that was launched by NASA in 2018. The Parker Solar Probe is designed to study the Sun's corona and its atmosphere in great detail, and it is equipped with a suite of instruments that measure the magnetic field solar wind, the corona's plasma, and the solar wind's acceleration. The Parker Solar Probe is also equipped with a suite of instruments that measure the magnetic field, the solar wind's acceleration, and the corona's plasma.

The Inouye Solar Telescope, which is located at the Mauna Kea Observatory solar observatory, is another important facility used in multi-messenger solar physics. The Inouye Solar Telescope is designed to study the Sun's corona and its atmosphere in great detail, and it is equipped with a suite of instruments that measure the magnetic field, the solar wind, the corona's plasma, and the solar wind's acceleration. The Inouye Solar Telescope is also equipped with a suite of instruments that measure the magnetic field, the solar wind's acceleration, and the corona's plasma.

In addition to these facilities, there are many other important facilities used in multi-messenger solar physics, such as the SOHO spacecraft, the Solar Dynamics Observatory, and the Hinode spacecraft. These facilities are designed to study the Sun's corona and its atmosphere in great detail, and they are equipped with a suite of instruments that measure the magnetic field, the solar wind, the corona's plasma, and the solar wind's acceleration.

One of the key challenges in multi-messenger solar physics is the need to coordinate the observations of these different facilities in order to obtain a complete picture of the Sun's behavior. This requires a coordinated effort between scientists from different countries and different scientific disciplines, as well as the development of new technologies and techniques to enable the sharing of data and information.

Another challenge in multi-messenger solar physics is the need to address the data analysis and interpretation of the data that is collected by these facilities. This requires the development of new algorithms and techniques to analyze the data and extract meaningful insights from it, as well as the development of new tools and techniques to visualize the data and make it accessible to a wider audience.

Despite these challenges, multi-messenger solar physics has made significant progress in recent years, and it has the potential to revolutionize our understanding of the Sun and its impact on the surrounding solar system. By studying the Sun's behavior and its impact on other celestial bodies in the solar system, scientists can gain a more comprehensive understanding of the Sun's role in shaping the structure of the heliosphere and the evolution of the solar system as a whole.

In conclusion, solar astronomy has a long history and has played an important role in shaping our understanding of the Sun and its impact on the surrounding solar system. The recent emergence of several significant observational facilities, such as the Parker Solar Probe, Solar Orbiter, and the Inouye Solar Telescope, among many others, is ushering in an exciting new era of scientific opportunities in multi-messenger solar physics. These facilities can address numerous pressing questions in contemporary solar physics, with a particular focus on their coordinated operation and the resulting synergies. Graduate students and researchers in solar physics will greatly benefit from the many new results presented within.

Weight: 440g
Dimension: 253 x 178 x 12 (mm)
ISBN-13: 9781009352888