Preface

*Solar System Planets and Exoplanets* describes planetary systems and their characteristics. Although the text focuses on the solar system, exoplanetary systems are also addressed. The book provides a current view of active planetary research areas with a focus on Mars and recent data and analysis from a variety of space probes.

Chapter 1 outlines the characteristics of solar system planets as well as their moons. The Asteroid Belt, Kuiper Belt, dwarf planets, comets, and meteoroids are also reviewed. An overview of exoplanets, their characteristics, and detection methods are summarized. The results of current and planned space probes, and their data-gathering capabilities are provided.

Chapter 2 describes historical, current, and future solar output characteristics. In particular, millennial oscillations of solar irradiance and magnetic field characteristics spanning the years 600–2600 are provided. This chapter discusses the consequences of these oscillations on the terrestrial atmosphere.

Chapter 3 focuses on Venus. Solar cycle variations in the position of vortex structures in the Venus wake are discussed. This chapter notes the interesting possibility that similar conditions should also be applicable to Mars, other bodies within the solar system, and exoplanets in external stellar systems.

Recent Mars data and associated observations are addressed in Chapters 4–8. Of particular interest are data that suggest the possibility that life could have existed on the planet's surface. The search for life on Mars is one of the main objectives of space missions and is the focus of Chapters 4–6. Technological advances in terms of operating aircraft on Mars (Chapter 7) and propulsion systems (Chapter 8) provide useful commentary regarding future innovations that will enhance upcoming space missions.

Chapter 4 covers sedimentation and algorithms to detect the possible existence of vegetation and humidity in the landing area of the Mars Exploration Rover-B (Opportunity). This chapter suggests the possibility of three types of water on the surface, as well as concentrations of neoxanthin, also on the landing area surface, that suggest the possible existence of microalgae.

Chapter 5 addresses the possibility of the existence of life on Mars. The chapter's morphological and morphometrical investigations suggest the presence of remnants of complex algal-like biota that could have lived on Mars.

Chapter 6 outlines new insights into the search for life on Mars. Analyses of data from a number of space probes suggest the possibility that life could have existed in the distant past of Mars, when its atmosphere was wetter and denser.

**II**

**Chapter 7 173**

**Chapter 8 191**

Asteroid Belt **209**

**Chapter 9 211**

Martian Moons and Space Transportation Using Chemical and Electric

Special Crater Types on Vesta and Ceres as Revealed by Dawn

The Challenge of Controlling a Small Mars Plane

*by Seiki Chiba and Mikio Waki*

Propulsion Options *by Bryan Palaszewski*

**Section 5**

*by Katrin Krohn*

The challenge of controlling a small aircraft on the surface of Mars is the topic of Chapter 7. This chapter discusses the control of an aircraft exploring the surface of Mars using dielectric elastomers. A structural model is developed for a wing having a control surface, and a wind tunnel test is completed.

Chapter 8 addresses the utilization of chemical and nuclear electric propulsion for the exploration of the Martian moons. The moons, Phobos and Deimos, have potential resources for refueling future space vehicles. The use of in situ resources has the potential to significantly reduce the dependence on Earth's resources on space vehicle propellants, liquid water, and breathing gases. These local resources offer the potential for space missions beyond Mars, and they offer a significant option for deep space exploration.

Chapter 9 covers unique features of asteroid belt bodies Vesta and Ceres. Special crater types, as revealed by the space probe Dawn, are the topic of this chapter. This chapter presents the three most characteristic crater forms found on both bodies.

The author acknowledges the assistance of Jelena Germuth and Anja Filipović for their assistance during the early stages of this book's development. Sara Debeuc is especially acknowledged for her kind assistance throughout the development, review, and finalization of this work. Her efforts significantly contributed to the finalization of this book.

> **Joseph Bevelacqua** Bevelacqua Resources, Richland, WA, USA

> > **1**

Section 1

Introduction

Section 1 Introduction

**3**

**Chapter 1**

**Abstract**

and Kuiper Belt

**1. Introduction**

Exoplanets

*Joseph Bevelacqua*

probes to gather additional data.

System planets as well as exoplanets [1–35].

icy bodies developed beyond the Asteroid Belt.

of significant atmospheres.

Solar System Planets and

Solar System planets have been studied for centuries, but the observation of exoplanets is only a few decades old. Consequently, knowledge of exoplanets is considerably more limited than Solar System planets. This chapter reviews the essential characteristics of Solar System planets and associated data derived from a variety of observational approaches. Exoplanet characteristics and their comparison to Solar System planets are provided as well as general detection methods and planned

**Keywords:** Solar System planets, Exoplanets, Dwarf Planets, Moons, Asteroid Belt,

Following the birth of the Universe through the Big Bang, a cyclic creation, or another unique event, space was filled with nebulae composed primarily of gas and dust. Stars formed from this primordial material, and the residual mass or interstellar medium (ISM) formed the constituents that led to planet formation. There are numerous papers, references, and books describing the characteristics of Solar

This crude model for planetary formation is based on the assumption that a star forms from the gravitational attraction and associated collapse of the primordial material. The contraction of the star with its decreasing radius increased the angular momentum of the accretion disk of ISM that formed around the star [3, 7, 10, 15]. The temperature of the material within the accretion disk varied with distance from the star. This temperature dependence caused rocky bodies to form throughout the disk, but icy bodies developed at greater distances. In the Solar System, the

Within the Solar System, the terrestrial planets formed from rocky bodies (i.e., preplanetary clusters also known as planetesimals). The terrestrial planets include Mercury, Venus, Earth, and Mars. The larger planets (i.e., Jupiter, Saturn, Uranus, and Neptune) formed from the rocky bodies, icy bodies, gas, and dust that led to their increased size. The higher temperatures and lower masses of the terrestrial planets limited their capture of gases. This was not the case for the giant planets. For Jupiter and Saturn, the larger masses and cooler temperatures led to the capture

The initial planet structures also developed their own accretion disks that led to the formation of planetary moons. These disks were larger for the giant planets,
