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Extra-Solar Planetary Systems

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Solar System Astrophysics

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Abstract

In this chapter we expand our view to include planetary systems beyond our own. We begin with the historical searches for planets around other stars to the present day, then survey the methods used to detect and study extra-solar planets (aka exoplanets), and discuss several of the historically important as well as some of the more interesting cases. We tackle the thorny question of how to define a planet (and a star, and of those intermediate objects, brown dwarfs). We reexamine the origin and stability of the solar system in this wider context, and conclude with a discussion of habitable zones, our own, in particular.

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Notes

  1. 1.

    The term “metals” in astrophysics frequently, as here, refers to all elements heavier than hydrogen and helium.

  2. 2.

    Rossiter (1924); McLaughlin (1924). During the 2012 transit of Venus, Molaro et al. (2013) succeeded in detecting the Rossiter-McLaughlin effect as Venus transited the Sun’s disk. They used the HARPS spectrograph on the 3.6-m ESO telescope. They observed the partial Venus eclipse in the light of the Sun reflected in the Moon. The transit of Venus across the receding solar hemisphere produced a modulation in the radial velocity with a negative amplitude of ≈−1 m s−1, in agreement with the theoretical model. The change in RV is comparable to the solar jitter and ≲1/2 that detected in the RV profiles of hot Neptunes, for example.

  3. 3.

    Lunine (2005, p. 88) makes a strong case that because of its multivalent nature, carbon can be involved in many more structures and varieties of structures than other relevant elements that it is far more suitable as a basis for biochemistry than, say, silicon.

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Authors and Affiliations

  1. Dept. Physics & Astronomy, University of Calgary, Calgary, Alberta, Canada

    Eugene F. Milone (Professor Emeritus) & William J. F. Wilson (Senior Instructor Emeritus)

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Challenges

Challenges

  1. [16.1]

    Plot the eccentricities of the objects in Table 16.2 vs. their semi-major axes. What can you conclude about the process of orbital circularization for these systems?

  2. [16.2]

    Now perform the same test for the objects in Table 16.3. What can you conclude about the process of orbit circularization for these systems? Can you account for the differences between the plots?

  3. [16.3]

    Examine the spectral types associated with each star in Table 16.1 with one or more planets. Can you draw any conclusions about the type(s) of star likely to have planets? Justify your response.

  4. [16.4]

    Compute the Roche limit and the synchronous orbit radius for the three closest planets in Table 16.2. You may need to look up data and make assumptions to do the computation, so name all sources and state all assumptions. Are these planets stable against tidal disruption at present or in the foreseeable future?

  5. [16.5]

    Compute the equilibrium temperature of HD 209458b and calculate the expected pressure scale height of its upper atmosphere; compare these values to those of Jupiter. Again, you may need to look up data and make assumptions to do the computation, so name all sources and state all assumptions.

  6. [16.6]

    For the case of HD 209458b, compute the true and Table 16.2 values of M sin i and a (see Sects. 16.2.1 and 16.4).

  7. [16.7]

    From the methods you have learned in the course of reading Solar System Astrophysics, and the data given in this chapter, calculate the brightness of the proposed planet in the alpha Centauri B system in, say, V magnitude, and suggest how it could be imaged.

  8. [16.8]

    Compute the “Hill radius”, the distance from a planet beyond which a satellite would be dominated by the star, for the “hot Jupiter” in the HD 209458 system. Compare the Hill radius with the Roche limit of the planet, to determine if such a planet could retain a moon.

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Milone, E.F., Wilson, W.J.F. (2014). Extra-Solar Planetary Systems. In: Solar System Astrophysics. Astronomy and Astrophysics Library. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-9090-6_7

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