DDA 2015 – Tidal Effects in Late Stage Accretion

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Session: Planet Formation II

Kevin Graves (Purdue)


We model the effects of tidal dissipation in the late stages of planetary accretion. We investigate the tidal dissipation during close encounters between embryos and nearly-formed planets using a modified version of the N-body integrator SyMBA. We calculate a total energy lost due to tides per close encounter and estimate the change in velocities of the bodies at each encounter. We measure the effects on the dynamics, evolution, and final outcome of the planets. Our initial results show a clear separation between the tidal and non-tidal case for a relatively strong tidal dissipation factor. We compare these results to traditional late stage simulations both with and without fragmentation.


  • Overview of late-stage terrestrial planet accretion
    • a few dozen embryos
    • a few thousand planetesimals
    • Morby 2012
    • giant plant migration?
      • increases AMD of inner solar system
      • must therefore start with a lower deficit
    • AMD: Jacobson & Morbidelli 2014
  • Tidal effects on planetary embryos
    • Lots of heat generation from various processes $\rightarrow$ magma oceans
    • Simple model for energy loss during a close encounter (Kaula & Harris 1973): tides
      • free parameters: tidal Love numbers, dissipation param
    • combine to a “tidal parameter”: $\frac{h_2 (k_2 + 1)}{Q}$
    • Tidal effects in an n-body integrator
      • no tides vs. strong tides:
        • plot: mass concentration (Chambers 2013) vs AMD
        • strong tides: higher mass concentration with AMD
        • weak tides: inverse

DDA 2015 – The Formation of Terrestrial Planets from the Direct Accretion of Pebbles

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Hal Levison (SwRI)


Building the terrestrial planets has been a challenge for planeVormation models. In particular, classical theories have been unable to reproduce the small mass of Mars and instead predict that a planet near 1.5 AU should roughly be the same mass as the Earth (Chambers 2001, icarus 152,205). Recently, a new model, known as ‘slow pebble accretion’, has been developed that can explain the formation of the gas giants (Levison+ 2015, Nature submitted). This model envisions that the cores of the giant planets formed from 100 to 1000 km bodies that directly accreted a population of pebbles (Lambrechts & Johansen 2012, A&A 544, A32) – centimeter- to meter-sized objects that slowly grew in the protoplanetary disk. Here we apply this model to the terrestrial planet region and find that it can reproduce the basic structure of the inner Solar System, including a small Mars and a low-mass asteroid belt. In particular, our models show that for an initial population of planetesimals with sizes similar to those of the main belt asteroids, slow pebble accretion becomes inefficient beyond ~1.5 AU. As a result, Mars’s growth is stunted and nothing large in the asteroid belt can accumulate.


  • Standard view:
    • disk forms, dust settles to midplanet
    • dust accumulates, ~1-10 km
    • runaway growth
    • oligarchic growth
    • late-stage
      • violent endgame for terrestrial planets
    • main problem: Mars is way to small
  • possible solution: pebble accretion
    • dust
    • settling dust creates turbulence
    • ~10 mm – 1 m pebbles
    • large planetesimals can accrete pebbles very effectively
      • strong gas drag $\rightarrow$ huge collision cross section (~Hill sphere)
  • Can this explain the low mass of Mars?
    • low-pebble-mass exponential cutoff
      • encounter time too short
    • A Ceres can grow if $r \lt \sim 1$ AU, but it can’t grow if $r \gt \sim 1$ AU.
    • $\rightarrow$ leaves ~20 planets inside of ~1 AU
    • subsequently very unstable and < 1 AU largely clears out
    • leaves behind essentially the Solar System architecture

DDA 2015 – Did our Solar System once have a STIP?

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Brett Gladman (CITA)


Continuing the established tradition in the field of speculative “fairy tales”, we postulate that our Solar System once had a set of several additional Earth-scale planets interior to the orbit of Venus. This would resolve a known issue that the energy and angular momentum of our inner-planet system is best explained by accreting the current terrestrial planets from a disk limited to 0.7-1.1 AU; in our picture the disk material closer to the Sun also formed planets, but they have since been destroyed. By studying the orbital stability of systems like the known Kepler systems, Volk and Gladman (companion abstract) demonstrate that orbital excitation and collisional destruction could be confined to just the inner parts of the system. In this scenario, our Mercury is the final remnant of the inner system’s destruction via a violent multi-collision (and/or hit-and-run disruption) process.This would provide a natural explanation for Mercury’s unusually high eccentricity and orbital inclination; it also fits into the general picture of long-timescale secular orbital instability, with Mercury’s current orbit being unstable on 5 Gyr time scales. The common decade spacing of instability time scales raises the intriguing possibility that this destruction occurred roughly 0.6 Gyr after the formation of our Solar System and that the lunar cataclysm is a preserved record of this apocalyptic event that began when slow secular chaos generated orbital instability in our former super-Earth system.


  • Motivation
    • inner edge of terrestrial planet zone
    • Mercury is weird.
    • Why don’t we have a STIP (system of tightly-packed inner planets)?
  • Mercury:
    • surfing the edge of secular chaos
    • not clear how it got to $e^2 + i^2 \sim (0.25)^2$
    • tough to strip mantle without it quickly falling right back
    • Ausphaug & Reiner (2014): Mercury is the end state of a sequence of collisions.
  • Why is there an inner edge?
    • Wetherill 1978 (Protostars & Planets): E and L of terrestrial planets requires an inner edge ~0.6 AU.
    • Historical way out: it’s too hot.
      • But modern studies indicate $T < 1500$K until much later.
  • If there is (collision) debris, where does it go?
    • radiation pressure: days
    • PR drag: kyr
    • meteoritic transfer: kyr-Myr
    • planetary interactions: ~10 Myr
    • $\rightarrow$ disappears quickly
    • if self-collisional, it will still disappear quickly
  • Secular architecture rearrangement
    • pump up to large $e$
    • fast collisions (~50 km/s)
      • vapor production
      • “bullet factory” — erosion of remnants
  • Meng et al. 2014 (Science)
    • spike of hot dust around young star
    • decay ~1 yr

DDA 2015 – On the Robust Production of Super Earths and Suppressed Emergence of Gas Giants in Dynamically Evolving Protostellar Disks

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Session: Planet Formation I

Doug Lin (UC Santa Cruz) (Brouwer award winner)


Radial velocity and transit surveys indicate the presence of super Earth around half of the main sequence stars regardless of their mass and metallicity. In contrast, the frequency of gas giants is much lower and increases with stellar mass and metallicity. I will show how the emergence of super-Earth is a robust process whereas the formation of gas giant planets is a threshold phenomena. The topics to be discussed include physical barriers in the planet building process, the role of migration in their evolving natal disks, planets’ interaction with each other and with their host stars. I will also discuss some key observations which may provide quantitative tests for planet formation theories.


  • Observed properties of exoplanets: Howard 2013 (Science)
  • Showstoppers:
    • disk formation
    • grain growth: the “meter barrier”
      • Trapping of refractory grains beyond the magnetospheric cavity
      • Tends to pile up at boundary
    • grain growth: the “kilometer barrier”
      • collisional fragmentation vs. grav.
      • oligarchic barrier: isolation mass
        • typically very small
    • embryo retention barrier — Type I migration
      • planet-disk tidal interaction
      • get to high mass $\rightarrow$ migrate outward
      • resonant sweeping $\rightarrow 2^{nd}$ generation
    • core barrier: embryo resonant trapping
      • bypass the resonant barrier
        • inner scattered outward, outer scattered inward $\rightarrow$ collisions $\rightarrow$ impacts of super Earths
    • gas accretion barrier
      • Is there a threshold mass for gas accretion?
      • runaway accretion
        • Why didn’t this happen for observed super Earths?
      • plenty of material left over: why didn’t they turn into gas giants?
      • Measured disk accretion rate…?
      • metal rich stars: no observed dependence, despite theory
        • But metallicity of star and disk need not be the same.
    • Rapid growth of proto gas giants
    • grand design barrier: dynamical instability
      • How did gas giants acquire their eccentricities?
      • Type II migration
        • provides constraint on growth process
      • Why did hot Jupiters stop their inward migration?
  • Close in planets
    • e.g. Kepler-78
      • 8-hour period
      • Star is magnetic
        • ~15 g
        • analogous to Jupiter-Io
        • induced EMF (unipolar induction) $\rightarrow$ energy dissipation at expense of planet’s orbit
        • Planet surface cannot be iron; must be silicates.
        • Flux tube footprints on star should move at period of planetary orbit, not stellar rotation.
  • Many other issues!

DDA 2015 – Inclination Excitation in Compact Extrasolar Planetary Systems

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Juliette Becker (U. Michigan) (Duncombe prize winner)


The Kepler Mission has detected dozens of compact planetary systems with more than four transiting planets. This sample provides a collection of close-packed planetary systems with relatively liRle spread in the inclination angles of the inferred orbits. We have explored the effectiveness of dynamical mechanisms in exciting orbital inclination in this class of solar systems. The two mechanisms we discuss are self-excitation of orbital inclination in initially (nearly) coplanar planetary systems and perturbations by additional unseen larger bodies in the outer regions of the solar systems. For both of these scenarios, we determine the regimes of parameter space for which orbital inclination can be effectively excited. For compact planetary systems with the observed architectures, we find that the orbital inclination angles are not spread out appreciably through self-excitation, resulting in a negligible scaRer in impact parameter and a subsequently stable transiting system. In contrast, companions in the outer solar system can be effective in driving variations of the inclination angles of the inner planetary orbits, leading to significant scatter in impact parameter and resultantly non-transiting systems. We present the results of our study, the regimes in which each excitation method – self-excitation of inclination and excitation by a perturbing secondary – are relevant, and the magnitude of the effects.


  • Why so many multi-planet transiting system?
  • Ballard & Johnson 2014, Ballard 2014, Morton 2014, Morton & Winn 2014
  • Seems to be a “Kepler dichotomy”
  • $\rightarrow$ inclination excitation important
  • $2^{nd}$ order secular Laplace-Lagrange theory (Murray &Dermott)
    • inc. & ecc. decoupled
    • Inclination as function of time (analytical)
  • Use Kepler 4+ planets as model systems
  • Conclusions:
    • Self-excitation in compact solar system planets does not appear to be a significant mechanism
    • Current Kepler systems with non-transiting planets could have started out transiting but driven out of transit by self-excitation
    • Excitation by compact solar system planets themselves (smear their mass into a disk) does notappearto be a significant mechanism
      • It might be possible to see multi-transiting systems with Jovian masses (if they exist)
    • Dynamical transit duration variations due to secular interactions will be small ($10^{-4}$ to $10^{-7}$ sec) but potentially observable (via statistics on long time series)

DDA 2015 – Secular Star-Disk Coupling and the Origin of Exoplanetary Spin-Orbit Misalignments

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Christopher Spalding (CalTech) (Duncombe prize winner)


A recent paradigm shift in exoplanetary astronomy has come with the detection of a substantial number of planets possessing orbits that are misaligned with respect to the spin axes of their host stars. Moreover, observations of misalignments now include coplanar, multi-transiting systems, suggesting that these planets inherited their orbital planes from a protoplanetary disk which was once itself inclined with respect to the star. It has been proposed that mutual star-disk inclination may arise as a consequence of turbulence within the collapsing molecular cloud core, out of which both the star and its disk form. Alternatively, misalignments may be aRained later on, through secular interactions between the disk and companion stars. In this work, we examine the secular dynamics of the stellar spin axis arising in response to the gravitational and accretional torques communicated between the star and its disk throughout the epoch of star and planet formation. Our analysis shows that even though the disk forms from turbulent material, and is thus expected to exhibit a stochastic variation in its orientation with time during the star formation process, gravitational disk-star coupling adiabatically suppresses the excitation of mutual star-disk inclination under all reasonable parameter regimes. As such, the excitation of mutual star-protoplanetary disk inclination must occur later on in the disk’s lifetime, by way of an encounter with a secular resonance between stellar precession and the gravitational perturbations arising from an external potential, such as a binary companion.


  • Motivation: our solar system, Laplace 1796
    • Ecliptic disk oriented approx perp to Sun’s spin axis
    • Goldreich & Tremaine 1980:
      • disk-driven migration
      • Jupiters eaten by stars
        • Why aren’t observed hot Jupiters eaten?
    • $\rightarrow$ hot Jupiters should be aligned with their disks
    • But significant fraction is seriously misaligned!
      • Tends to be more massive planets
  • How to getmisalignments?
    • Disk-driven migration doesn’t work
    • High-eccentricity + tidal?
      • Cannot explain multi-transiting misaligned systems (Huber et al. 2013)
  • $\rightarrow$ Are disks really aligned with their stars?
  • Hypothesis 1: misalignment during formation
    • Spalding et al. 2014 (ApJ)
    • Cores are turbulent
    • Spin dir varies randomly by $\approx30^{\circ}$ every ~0.01 pc
    • Shell infall time $\approx 10^4$ yr
    • Disk adopts plane of whatever shell falls last (Bate et al. 2010)
    • Star-disk system forms misaligned
    • BUT: disk-star coupling?
      • Young stars spin rapidly $\rightarrow$ oblate
        • Dynamically equivalent to massive wire around point mass
        • $\rightarrow$ disk precession
      • Use Laplace-Lagrange secular theory
        • Disk annuli act as outer perturbers upon stellar irientation
        • $\rightarrow$ precession period ~100 years(!)
    • Numerical simulation — will star spin axis follow motion of disk?
      • Star trails disk, even though motion stochastic
  • Hypothesis 2: binary companion in orbit around star+disk — disktorquing
    • Companion causes $\gg 10^4$ yr precession
    • Star-disk coupling weakens with time
      • mass loss
      • stellar contraction
    • Spalding & Batygin 2014 (ApJ)
    • Eventually, disk-binary precession ~ star-disk precession
      • hits secular resonance, catapulting disk/star into retrograde orbits
    • Final inclination only depends upon initial binary inclination
  • Summary:
    • Gravitational star-disk coupling prevents misalignment early on.
    • Neighboring stars excite misalignments by was of a secular resonance.
    • Misalignments are consistent with disk-driven migration.

DDA 2015 – MMRs and the Origins of Extrasolar Orbital Architectures

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Konstantin Batygin (CalTech)


The early stages of dynamical evolution of planetary systems are often shaped by dissipative processes that drive orbital migration. In multi-planet systems, convergent amassing of orbits inevitably leads to encounters with rational period ratios, which may result in establishment of mean motion resonances. The success or failure of resonant capture yields exceedingly different subsequent evolutions, and thus plays a central role in determining the ensuing orbital architecture of planetary systems. In this talk, we will show how an integrable Hamiltonian formalism for planetary resonances that allows both secondary bodies to have finite masses and eccentricities, can be used to construct a comprehensive theory for resonant capture. Employing the developed analytical model, we shall examine the origins of the dominantly non-resonant orbital distribution of sub-Jovian extrasolar planets, and demonstrate that the commonly observed extrasolar orbital structure can be understood if planet pairs encounter mean motion commensurabilities on slightly eccentric (e ~ 0.02) orbits. Accordingly, we speculate that resonant capture among low-mass planets is typically rendered unsuccessful due to subtle axial asymmetries inherent to the global structure of protoplanetary disks.


  • SeeMécaniqueCéleste, Laplace 1805!
    • But origins not really understood until Roy & Ovenden 1954, Goldreich 1964 (MNRAS)
  • Disk-satellite interactions (Goldreich & Tremaine)
  • But what about more than one planet?
  • All tend to migrateinward then lock intoMMRs (Pierens 2013 A&A)
    • $\Rightarrow$ numerical models predict MMR lock
    • BUT only ~15% of observed planet pairs are in resonance
  • The real Hamiltonian (planet-planet interactions) is actually probably a mess.
    • See Poincare’s book, vol. 2(!)
    • Define a canonical rotation that gives an integral of the motion (“generalized reducing transformation” –Poincare)
      • Basically, a generalized Tisserand parameter
    • Batygin & Morbidelli 2013(?)
  • An analytical theory for resonant capture: unrestricted ETB problem.
    • Batygin 2015 (MNRAS, submitted)
    • Capture prob. only depends on total mass of the planets, NOT the mass ratio
      • phase space area occupied by planet is small
    • Kepler sample: critical eccentricity is ~0.02 — very small!
      • Larger than this, capture fails
      • Matches observed value!
    • Explains Jupiter-Saturn MMR lock
    • Perhaps slight deviations from axial symmetry in protoplanetary disks are responsible for the orbital architecture we observe today.

DDA 2015 – Consolidating and Crushing Exoplanet Systems

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Kathryn Volk (U. British Columbia)


Kepler revealed the common existence of tightly-packed planetary systems around solar-type stars, existing entirely on orbits with periods shorter than ~200 days. Those systems must have survived for the ages of their host stars (~5 Gyr), so their formation mechanism must provide inter-planet spacings that permit long-term stability. If one postulates that most planetary systems form with tightly-packed inner planets, their current absence in some systems could be explained by the collisional destruction of the inner system after a period of meta-stability. The signatures of such intense collisional environments may have been observed around stars in the form of rapidly varying debris disks; in these observed disks, collisional products are being disposed of via drag down onto the star or grinding to the nearly instantaneous dust blow-out limit. We use the orbital spacings and planet masses of the observed Kepler multi-planet systems to investigate the stability and long-term behavior of the systems. We find that many of our Kepler system analogs are unstable on 100 Myr timescales, even for initially small eccentricities (0-0.05); the instability timescales in these systems are distributed such that equal fractions of the systems experience planetary collisions in each decade in time. We discuss the likely outcomes of collisions in these systems based on the typical collision speeds from our numerical integrations and what implications this has for interpreting the observed Kepler multi-planet systems. The possible implications for our Solar System are discussed in a companion abstract (Gladman and Volk).


  • Architectures of close-in (closely packed) planetary systems (from Kepler)
  • Fabrycky 2014
  • ~5-10% ofFGK field stars
    • These systems must be stable on Gyr timescales
  • Are all stars formed tightly packed?
  • Modeled 13 such Kepler systems
    • Preserved $a$ and masses, orbital angles randomized
    • Allowed $e_0$ to vary $0 < e_0 < 0.05$
    • Sudden onset of instability in 11 of these 13 after tens to ~100 Myr
      • [why is she surprised?]
    • These eccentricities are in range of observed values
    • Decay rates consistent with e.g. Holman & Wisdom (1992 AJ)
  • Why sudden onset?
    • History is very sensitive to ICs [duh]
    • Consolidation (low-speed collisions) vs. Destruction (high-speed collisions)
    • First collision is often near the accretion/erosion boundary — i.e., low-speed
    • Masses in 4-5 planet systems tend to be lower, while individual masses in ~3-planet systems are higher: mergers?
    • Tracked collision speeds during integrations.
    • Second collision often goes into erosion regime (i.e., high-speed)
      • Observing debris should be rare (but see Meng et al. 2012)
    • Ergodicity allows large variety of outcomes
  • $\Rightarrow$ tightly packed systems could be ubiquitous initially
    • Young stars should show higher fraction
  • The remaining ~95% should be 0-2 planet systems

DDA 2015 – Capture into Mean-Motion Resonances for Exoplanetary Systems

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Session: Exoplanet Theory II

Maryame El Moutamid (Cornell)


Many bodies in the Solar System and some exo-planets are close to or captured in Mean Motion Resonances (MMR). Capture into such resonances has been investigated by many authors. Indeed, the Hamiltonian equations of motion in presence of migration are given by Sicardy and Dubois Cel. Mech. & Dyn. Astron., 86, 321-350 (2003). Fleming and Hamilton, Icarus 148, 479-493 (2000), studied the problem in a less generic context. In these two papers, the authors studied the problem of 1:1 corotation (Lagrange points L4 and L5), rather than m+1:m corotations (El Moutamid et al, Cel. Mech. & Dyn. Astron, 118, 235-252 (2014)). We will present a generic way to analyze details of a successful (or not) capture in the case of an oblate (or not) central body in the context of Restricted Three Body Problem (RTBP) and a more General Three Body Problem in the context of known statistics for captured exoplanets (candidates) observed by Kepler.


  • Captures partial near MMR (Fabrycky et al. 2012)
  • No generic study on coupling between associated resonances (ERTB vs. general TB)
  • 1) simple model,2DoF — $(m+1) n’ \approx m n$
    • splitting the corotation and Lindblad resonances (by $J_2 \neq 0$)
    • Lindblad: vary $e$
    • corotation: pendular motion (conserves $e$)
    • plot: $J_c – J_L$ vs. $\phi_C$
  • 2) general case
    • can define a constant of motion: $J_{c,relat} = \frac{A^2 \xi}{m} – \frac{A’^2 e’}{m+1} – ?? = const.$
  • Add dissipationforMMR capture
    • ratio: potential barrier of one vs. other body
    • plot: potential energy vs. critical angle of corotation
    • probability of capture: very very small

DDA 2015 – Obliquity Evolution of Earth-Like Exoplanets in Systems with Large Inclinations

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Russell Deitrick (U. Washington)


In order to properly assess the potential for habitability and prioritize target selection for the characterization of exoplanets, we need to understand the limits of orbital and rotational dynamics. Large satellites may be rare and very difficult to detect. Consequently, it is necessary to quantify the likelihood of a planet’s having extreme obliquity cycles in the absence of a moon and to model the potential impact on the planet’s climate. We explore the obliquity evolution of (1) known exoplanet systems that could contain Earth-like planets in the habitable zone and (2) hypothetical planets in mutually inclined, chaotic resonant configurations that experience some of the most extreme orbital evolution possible. We use a secular obliquity model coupled to either an N-body models or a 4 order secular orbital model. We find that in some known systems, planets’ obliquity variations are small and unlikely to have a major effect on climate, unless undetected planets are present. Systems with three or more planets are significantly more dynamically rich, with planets that undergo obliquity changes of ~10° over 50,000 years and >30° over a few million years. In resonant configurations, Earth-like exoplanets can undergo dramatic and chaotic evolution in eccentricity and inclination while remaining stable for over 10 Gyr. In configurations in which eccentricities and inclinations stay below ~0.1 and~10°, respectively, obliquities oscillate quasi-periodically with amplitudes similar to the non-resonant, three-planet configurations. In more dynamically active configurations, in which eccentricities and inclinations evolve to e > 0.3 and i > 15°, obliquities can extend from ~0° to well past 90°. In extreme cases eccentricities can reach >0.9999 and inclinations >179.9 degrees, driving precession rates in excess of degrees per year. However, these planets can graze or impact the stellar surface and are probably not habitable.


  • $\upsilon$Andromedae c and d
    • obliquity oscillations
  • Model description
    • Barnes, Deitrick et al. 2015
    • Using the secular disturbing function (Murray & Dermott) and a secular obliquity model (Kinoshita 1975, 1977)
    • HD190360
      • obliquity varies w large amplitude in a “strip” in $\Delta i_0$ – $e_0$ plane — WTH?
      • two planets interacting (an Earth and a super-Jupiter) … somehow
      • Inside the “strip”, a commensurabilitylibrates
        • $(\varpi’ – \varpi) – (\Omega + p_A)$
        • outside the “strip”: no libration
      • Analogous to a compound pendulum
  • Summary
    • Non-coplanar systems in MMR exhibit long-lived chaos.
    • These systems can be formed by scattering.
    • Possible way to form misaligned hot Jupiters.
    • Earth-like planets in these systems can also have chaotic obliquity variations.

DDA 2015 – Loners, Groupies, and Long-term Eccentricity Behavior – Insights from Secular Theory

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Christa Van Laerhoven (CITA)


Considering the secular dynamics of multi-planet systems provides substantial insight into the interactions between planets in those systems. Secular interactions are those that don’t involve knowing where a planet is along its orbit, and they dominate when planets are not involved in mean motion resonances. These interactions exchange angular momentum among the planets, evolving their eccentricities and inclinations. To second order in the planets’ eccentricities and inclinations, the eccentricity and inclination perturbations are decoupled. Given the right variable choice, the relevant differential equations are linear and thus the eccentricity and inclination behaviors can be described as a sum of eigenmodes. Since the underlying structure of the secular eigenmodes can be calculated using only the planets’ masses and semi-major axes, one can elucidate the eccentricity and inclination behavior of planets in exoplanet systems even without knowing the planets’ current eccentricities and inclinations. I have calculated both the eccentricity and inclination secular eigenmodes for the population of known multi-planet systems whose planets have well determined masses and periods. Using this catalog of secular character, I will discuss the prevalence of dynamically grouped planets (‘groupies’) versus dynamically uncoupled planets (‘loners’) and how this relates to the exoplanets ‘long-term eccentricity and inclination behavior. I will also touch on the distribution of the secular eigenfreqiencies.


  • Secular character of multi-planet system
  • planet-planet interactions
  • only need masses and semimajor axes (not eccentricity, not inclination) to set secular structure
  • two-planet system: two eccentricityeigenmodes
    • $h = e \sin \varpi$, $k = e \cos \varpi$ plot: $e$ is a vector
    • each $e$ vector is the sum of two eigenvectors
  • 3-planet system: “groupie”-ness and loners
    • groupies:
      • $e$ highly variable
      • $\varpi$ precession not uniform
    • loners:
      • $e$ does not vary by much
      • $\varpi$ precesses steadily
  • Kepler-11
    • outer planet is a loner — does not interact with others
    • 5 inner planets are groupies — interact strongly with each other
  • Summary: most planets are “groupies”, “loners” are rare.

DDA 2015 – Using Populations of Gas Giants to Probe the Dynamics of Planet Formation

This is one of a series of notes taken during the 2015 meeting of the AAS Division on Dynamical Astronomy, 3-7 May, at CalTech. An index to this series (all the papers presented at the meeting) is here.

Session: Exoplanet Theory I

Ruth Murray-Clay (UC Santa Barbara) (invited)




  • How do giant planets and brown dwarfs form?
  • Architecture of Solar System is atypical.
  • Lots of gas giants at large distances, small distances (“hot Jupiters”), but not much in between a la Solar System. Why?
  • SS: rocky planets (~1 AU), gas giants (~5-10 AU), ice giants (~20-30 AU)
  • Theory: cannot predict numbers, but can predict patters in system architectures and statistical populations
  • How to get companions to stars: 1) turbulent fragmentation, 2) grav. instability, 3) core accretion
  • HR8799: testbed for planet formation theories
    • 4 Jupiter-mass planets
    • turbulent frag.? No: system is not hierarchichal
    • grav. inst.?
      • iffy – minimum fragment distance problems (but could have migrated)
      • Timing – collapse must occur at end of infall or a binary star results
    • core accretion?
      • dynamical (growth) timescale is too long ($t_{grow} > t_{infall}$)
      • $t_{grow} > t_{disk}$
      • cross section regimes — all problematic:
        • physical cross section
        • grav focusing
        • gas drag capture
  • Make gas useful.
    • no gas: particles can orbit inside core Hill radius
    • gas: “wind shear”
      • binary capture
      • particle capture can occur out to Hill radius
      • growth time at 70 AU can be short enough to nucleate an atmosphere
      • turbulent gas: okay
    • accretion cross sections increase by up to $10^4$
  • Gemini Planet Imager could confirm this theory.
  • Metal-rich stars hostmorehotJupiters and highly eccentric planets: signature of planet-planet interactions? Why?
    • Scattering?
    • Secular chaos?
    • Perhaps those systems form many Jupiters.
  • Are the solar system analogs orbiting low metallicity stars?

The Printer and I: A Tale of Spinning Fans, Diseased Hearts, and the Tragedy that is Life

[Click to embiggen.]

This (see photo) is how I spent my afternoon and evening, today. I have a conference to attend next week and must present a poster paper on some recent research results. Because I know by now that both Old Man Murphy and Loki the Trickster always lie in wait, snickering — I hear you, you bastards — I go to check the large-format printer. It is a Beast, and it turns electrons into poster papers. I flip the power switch, and it makes a horrible noise, won’t boot up, freezes, then whines plaintively, “call HP … call HP … please, won’t you call HP ….” Not very encouraging. Screw you, Loki — thou art a Puck.

As with all things computer that misbehave, I keep trying the same thing over and over, hoping for a different result, though I know full well that no different result will … um … result. Indeed, no dice. Run around the building and check with everybody: nobody knows what’s wrong or what happened. Yeah, sure.

What to do? Go find some screwdrivers, of course. The horrible noise emanates from somewhere around the power supply. Sort of. It’s buried in the guts of the Beast, so it’s hard to tell from the outside. It is a place to start, anyway. I roll up the sleeves of my robe, pick up a Holy Implement of Torx, and get to work …

Several hours later, I finally have figured out, cuss word by cuss word (proper ordering is important), how to get past all the barriers cleverly designed by Evil HP Engineers to make rational disassembly near-impossible. (Ever disassemble a laptop computer, down to the bare metal? This is harder, I kid you not.) Sixty screws later (I count them, twice), I get to the power supply fan. The heart of the Beast is diseased, despoiled. It is not turning quite right, and the motor shaft wiggles a little. It is not supposed to wiggle. Even a little. Culprit apprehended at last? Perhaps. Fortunately, it’s just a cheap $8 cooling fan you can pick up at any Radio Shack.

But Radio Shack does not exist anymore. When did that happen?

We have come round to this place again: what to do? Rummage around in the junk spare parts room, of course. It is a glorious room, beloved of tinkerers on staff. Bingo: six salvaged computer power supplies, just lying there on a shelf, calling to me. No, seven! But I am wise to their siren song. One after another, a closer look reveals frightening ugliness — mostly in the form of caked-on dust and dirt and grime. Their hearts spin, but they are Unclean and Decrepit. Sigh … last one: yay, Cleanliness! The Blessed One, Savior of the Beast, is found.

It believes it has been bestowed a new chance at life. I wish I could be happy for it. Little does it know its fate. Surely it deserves to be told of its pending doom? Yet that would crush its new-found hopes. You are perverse and cruel, you Fates! I do not have the heart to tell it.

True to my calling as Lord High Tinkerer, I pick up the Holy Implement of Torx and sacrifice the Blessed One upon the Ancient Altar of Gorthung (a fifty-year-old, government-issue desk, solid and heavy as a tank, with an ice-cold slate top). I flay its body and cut out its heart. I know no mercy.

Fan in bloody hand (a blood blister acquired some time during printer pieces-parts separation has popped), I trundle down the hill to the electronics lab. There, a colleague — the Wizard of Wire, Lord of Circuit — performs minor surgery. Lo, and behold! Upon application of the Lightning of Zoltar (a 12-volt power supply), the heart of the Blessed One lives again, spinning round and round in a most pleasing whir. Back up the hill.

That dreaded niggle squatting in the back of my mind finds a crack and blossoms. It dawns on me: now I have to put it all back together. Sixty screws. I realize I am tired. I’ll never remember where they all go. Come back tomorrow with freshly caffeinated veins? Pffft. Such is for wusses, unbecoming of a Tinkerer. So, since the operation of my memory — even on a good day — resembles most closely that of a sieve, I have little choice but to re-figure out how to take apart the Beast but in reverse. I am reminded of Ginger Rogers. I miss Ann Richards and her rapier wit. Today is not a good day.

Another hour passes by. I wave hi. We do that a lot, Time and I. My finger leaks on the table; I wipe it. And also on the housing of the reassembled printer power supply. I look at the smear, and I do not wipe it. I have left my mark upon this Beast, I think to myself. I shall not remove it. It will be buried amidst your guts; only you and I will ever know it is there. This token of my toil is enough, I decide. I move on.

At last, it is back together, despite all the King’s men staying home, watching TV. I do not want to plug it in. I’m sure you understand. Don’t you? Even so, I still roll the Beast back to its lair. I reattach its stiff black tail. I notice it is dirty, the cord, this conduit of the Lightning of Zoltar.

We have arrived at the moment of truth: I flip the switch. And wait. As with a pot of water that has yet to boil, it is best not to stare at a booting computer, especially one as slow and dumb as the Beast’s. I stare anyway. I wave hi to passing Time again, then it whirs with a pleasing sound. And dies. And tells me to call HP.

Naturally, I turn it off, wait ten seconds (capacitors can be slow to bleed, you know), and then turn it on again. Maybe something different will happen this time.

math test

Here’s how to get MathJax up and running for your blog: part I, part II. The three tests below are text lifted from elsewhere.

Test 1

Consider first what we shall call the direct geometry case, in which we use only the zenith angle $z$ and bypass the geocentric angle $\theta$. The length of side $\overline{CM}$ follows from the right triangle $\widehat{CMP}$:

$$\begin{equation}\begin{array}[b]{ccl}\left(R+H\right)^{2} & = & \left(D\sin z\right)^{2}+\left(R+h+D\cos z\right)^{2}\\ \\ & = & D^{2}+\left(R+h\right)^{2}+2\left(R+h\right)D\cos z\end{array}\label{eq:R+H-test}\end{equation}$$


\begin{equation}D^{2}+2\left(R+h\right)D\cos z-\left[\left(R+H\right)^{2}-\left(R+h\right)^{2}\right]=0\label{eq:D eqn-test}\end{equation}

with solution

\begin{equation}\begin{array}[b]{ccl}D & = & -\left(R+h\right)\cos z\pm\sqrt{\left(R+h\right)^{2}\cos^{2}z+\left[\left(R+H\right)^{2}-\left(R+h\right)^{2}\right]}\\ \\& = & \left(R+h\right)\left(\sqrt{\cos^{2}z+\dfrac{\left(R+H\right)^{2}-\left(R+h\right)^{2}}{\left(R+h\right)^{2}}}-\cos z\right)\end{array}\label{eq:D soln quadratic ugly-test}\end{equation}

where the geometry of the problem requires the positive root. For convenience, define

\begin{equation}\epsilon\equiv\dfrac{H}{R}\quad\mathrm{and}\quad\xi\equiv\dfrac{h}{R}\label{eq:eps and xsi defs-test}\end{equation}

Then we can write eq. \eqref{eq:D soln quadratic ugly-test} as

\begin{equation}D=\left(R+h\right)\left(\sqrt{\cos^{2}z+\left(\dfrac{1+\epsilon}{1+\xi}\right)^{2}-1}-\cos z\right)\label{eq:D soln quadratic-test}\end{equation}

Eq. \eqref{eq:D soln quadratic-test} has the disadvantage of subtraction of two nearly equal numbers.

Test 2

We would like to know what is the radius $\bar{r}$ of the center of mass

of a grid cell of inner radius $r_{1}$ and outer radius $r_{2}$. In polar coordinates $\left(r,\theta\right)$ an infinitesimal area element is $dA=r\,dr\,d\theta$, so

\begin{equation}\bar{r}=\frac{1}{\Delta A}\intop_{0}^{\Delta\theta}\intop_{r_{1}}^{r_{2}}r\,dA=\frac{1}{\Delta A}\intop_{0}^{\Delta\theta}\intop_{r_{1}}^{r_{2}}r^{2}dr\,d\theta\label{eq: area-weighted r integral-test}\end{equation}

where $\Delta A=\frac{\Delta\theta}{2\pi}\cdot\pi\left(r_{2}^{2}-r_{1}^{2}\right)$.


\begin{equation}\Delta A=\frac{\Delta\theta}{2}\left(r_{2}^{2}-r_{1}^{2}\right)\label{eq: cell area-test}\end{equation}


\begin{equation}\bar{r}=\frac{1}{3}\frac{\Delta\theta}{\Delta A}\left(r_{2}^{3}-r_{1}^{3}\right)=\frac{2}{3}\frac{r_{2}^{2}+r_{1}r_{2}+r_{1}^{2}}{r_{1}+r_{2}}\label{eq: area-weighted r-test}\end{equation}


Thus, we have the bootstrapping scheme

\begin{equation}\begin{array}{rclcrcl}\bar{r}_{0} & = & \dfrac{2}{3\Delta^{2}}\left(r_{2,0}^{3}-r_{1,0}^{3}\right) & & r_{2,0} & = & \sqrt{r_{1,0}^{2}+\Delta^{2}}\\& \vdots & & & & \vdots\\\bar{r}_{k} & = & \dfrac{2}{3\Delta^{2}}\left(r_{2,\,k}^{3}-r_{2,\,k-1}^{3}\right) & & r_{2,\,k} & = & \sqrt{r_{2,\,k-1}^{2}+\Delta^{2}}\\& \vdots & & & & \vdots\\\bar{r}_{N_{r}-1} & = & \dfrac{2}{3\Delta^{2}}\left(r_{2,\,N_{r}-1}^{3}-r_{2,\,N_{r}-2}^{3}\right) & & r_{2,\,N_{r}-1} & = & \sqrt{r_{2,\,N_{r}-2}^{2}+\Delta^{2}}\end{array}\label{eq: bootstrap scheme}\end{equation}

where, again, we start with $r_{1,0}=r_{min}$ .

Test 3

Now, $-\widehat{z}\times{\left(\widehat{z}\times\overrightarrow{r}\right)}=\overrightarrow{r}-{\left(\widehat{z}\cdot\overrightarrow{r}\right)}\widehat{z}$, so


Define a new effective potential




Then we find the satisfying result


The individual components of \eqref{EQUATION.7aeaeb03-1226-46ab-815a-4b28e71a84a5} are

\begin{equation}\begin{aligned}x^{\prime\prime}-2y^{\prime} & =\frac{1}{{1+e_{p}\mathrm{cos}\mathrm{\theta}}}\frac{{\partial\mathrm{\Omega}}}{{\partial x}}\\y^{\prime\prime}+2x^{\prime} & =\frac{1}{{1+e_{p}\mathrm{cos}\mathrm{\theta}}}\frac{{\partial\mathrm{\Omega}}}{{\partial y}}\\z^{\prime\prime}+z\hspace{0.9em} & =\frac{1}{{1+e_{p}\mathrm{cos}\mathrm{\theta}}}\frac{{\partial\mathrm{\Omega}}}{{\partial z}}\end{aligned}\label{}\end{equation}


\begin{equation}\begin{array}{rcl}\overrightarrow{\nabla}\mathrm{\Omega} & = & \left[\begin{matrix}x-\dfrac{1-\mathrm{\mu}}{r_{1}^{3}}\left(x+\mathrm{\mu}\right)-\dfrac{\mathrm{\mu}}{r_{2}^{3}}\left(x-1+\mathrm{\mu}\right)\\y\left(1-\dfrac{1-\mathrm{\mu}}{r_{1}^{3}}-\dfrac{\mathrm{\mu}}{r_{2}^{3}}\right)\\z\left(1-\dfrac{1-\mathrm{\mu}}{r_{1}^{3}}-\dfrac{\mathrm{\mu}}{r_{2}^{3}}\right)\end{matrix}\right]\\ \\& = & \left(1-\dfrac{1-\mathrm{\mu}}{r_{1}^{3}}-\dfrac{\mu}{r_{2}^{3}}\right)\overrightarrow{r}-\mathrm{\mu}\left(1-\mathrm{\mu}\right)\left(\dfrac{1}{r_{1}^{3}}-\dfrac{1}{r_{2}^{3}}\right)\widehat{x}\end{array}\label{}\end{equation}