Aaron M. Geller
NSF Astronomy and Astrophysics Postdoctoral Fellow
Northwestern University & The Adler Planetarium
NGC 188 Image of the old (7 Gyr) open cluster NGC 188 taken at the WIYN 0.9m telescope; blue stragglers are circled.
Credit: K. Garmany, F. Haase NOAO/AURA

Research

Gravitational dynamics has stood as a foundation of astronomy since Sir Isaac Newton modified Kepler's third law to show that the motions of our planets can be described by orbits around a central force of gravity. Motion due to the effects of gravity is perhaps one of most relatable areas of physics, as we experience the influence of gravity on a daily basis. Stellar systems like open and globular star clusters offer a particularly rich dynamical environment, where two-body relaxation drives a relatively rapid evolution and close encounters between individual stars and binaries can occur on a regular basis.

Here you will find descriptions of a number of exciting research projects that my collaborators and I are pursuing to study the effects of stellar encounters on the evolution of multiple-star systems, planetary systems and star clusters, including many important projects for students. If any of these projects spark your interest, please contact me at the information given below.



Quick Links to Projects
WIYN Open Cluster Study (WOCS)
WIYNPhotograph of the back of the WIYN 3.5m telescope, showing the mirror actuators which push or pull on the back face of the mirror to maintain the best optical figure. The WIYN telescope is located on Kitt Peak near Tucson, Arizona.
Credit: A. M. Geller

The WIYN Open Cluster Study (WOCS). is a collaboration spanning more than a decade with members at over a dozen universities. The goals of WOCS are to obtain precise and comprehensive photometry, spectroscopy and astrometry for stars in open clusters spanning a wide range in age and metallicity. My primary contributions to WOCS have been stellar radial-velocities for thousands of stars in the open clusters:

Through our observations, we are defining the cluster member population and analyzing the spectroscopic binaries (binary fraction, frequency distributions of orbital parameters, mass ratios) for binaries with orbital periods approaching the hard-soft boundary. These observations also provide a comprehensive survey for anomalous stars, including secure establishment of their cluster membership. Importantly, these observed binary population provide essential guidance for sophisticated N-body open cluster simulations, from which we are studying how stellar encounters modify a population of binary and multiple-star systems and planetary systems, and influence the evolution of star clusters.

Recently we have added a few new open clusters to the survey, including two in the Southern Hemisphere:

These clusters (as well as M35) are all young, and therefore they provide important information about the near-primordial stellar populations in open clusters. Furthermore, these four clusters fill an important niche as a bridge between the Pleiades (100 Myr) and the Hyades (750 Myr), and will be used to relate both of these young and well-studied clusters and to search for evolutionary signatures. My personal interest lies in defining the binary populations in these clusters, specifically binary frequency and distributions of orbital parameters (e.g., period, eccentricity, mass ratio). These near-primordial binary populations provide essential, and hitherto unknown, guidance for defining the initial stellar populations in numerical N-body models.

Collaborators: UW WOCS group, full WOCS team

Papers: Geller et al. (2008, 2009, 2010, 2011), Hole, et al. (2009), Gosnell, et al. (2011)


Student Projects: Our surveys of M37, NGC 3532 and NGC 2516 are nearing their first milestone, having sufficient observations for important analyses to identify the cluster members and binaries and to search for exotic stars. Furthermore, both NGC 3532 and NGC2516 are within the field of the upcoming Large Synoptic Survey Telescope (LSST), which will revolutionize our understanding of the time-variable sky, and therefore these projects will have significant future impact.

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Cluster Membership
M35 radial-velocity histogramRadial-velocity (RV) histogram for stars in the field of M35. Cluster members are clearly identified by the sharp peak in the distribution at the mean RV of about -8 km/s. Stars in the Glactic field, not associated with the cluster, have a significantly broader RV distribution. The dashed lines show the simultaneous Gaussian fits to the cluster and field RV distributions. We use these Gaussian fits to calculate membership probabilites for each individual star in the cluster.
Credit: A M. Geller, et al. (2010, AJ)

Determining cluster membership is the fundamental first step to studying any star cluster. All members of a star cluster move with a very similar velocity (to within the cluster velocity dispersion, which is typically <1 km/s in open clusters), while field stars have a much wider range in velocities. Therefore analyzing the observed stellar radial-velocities (the primary product of our spectroscopic surveys) separates stars that are members of the cluster from interloping field stars that are actually in front of or behind the cluster. This analysis is particularly important, as many open clusters are found in or near the disk of our Galaxy, amidst a rich population of Galactic field stars.

I have personally determined radial-velocity membership probabilities for thousands of stars in the open clusters NGC 188, M35 and NGC 6819, and I am currently working on performing a similar analysis for stars in M67. We are poised to begin our membership analyses of M37, NGC 3532 and NGC 2516, which would be ideal short-term student projects. I am also involved in determining the cluster members of NGC 7789 and NGC 2516; these projects are led by graduate students at the University of Wisconsin - Madison.

Once cluster members are determined, we can explore a wide range of exciting projects, including studying the binary population (e.g., determining the binary frequency and distributions of orbital parameters) or identifying exotic stars like blue stragglers. We can even use these observations to guide sophisticated numerical simulations to study the past and future evolution of the cluster.

Collaborators: Bob Mathieu, Natalie Gosnell, Katelyn Milliman, Søren Meibom, David Latham, Sydney Barnes, David James, Hugh Harris

Papers: Geller et al. (2008, 2010), Hole, et al. (2009)


Student Projects: As mentioned above our surveys for M37, NGC 3532 and NGC 2516 are nearing their first milestone. Specifically we are close to having three or more observations of each star in our samples. We require at least three observations before determining a membership probability to ensure that we can identify binaries, whose radial velocities vary and therefore require further observations to calculate their true center-of-mass motion needed to determine cluster membership. An interested students can work with our data for one (or more) of these clusters to calculate each star's mean radial velocity, construct the distribution of observed radial velocities, and calculate each star's probability of cluster membership (see Figure on the right). Once members are identified you can, for instance, determine the cluster velocity dispersion, which enables you to estimate the mass of the cluster.

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Binaries and Multiple-Star Systems
Binary OrbitRadial-velocity (RV) as a function of orbital phase for the blue straggler binary ID 7782 in NGC 188. This particular binary is "double lined" meaning that we detect the flux from both stars in our spectra. The primary RVs are shown in the solid points, and the secondary RVs are shown in the open circles. The lines show the kinematic orbital solution. In the bottom panel, we show the RV residuals (observed - expected) .
Credit: A M. Geller, et al. (2009, AJ)

A binary companion star will pull on its partner as they both orbit about their mutual center of mass. This pull is detectable within a time series of radial velocities for a given star by examining the radial velocity standard deviation or through a chi-squared analysis. Given a long enough time baseline of observations for a binary, we can solve for the orbital solution to determine the period, eccentricity, mass ratio, etc. , which are particularly important for characterizing eclipsing binaries (like those that will be discovered by LSST) and for guiding sophisticated N-body open cluster simulations.

I have studied the binary population in the old open cluster NGC 188 in detail. In Geller et al. (2009) we present the kinematic orbits for 98 binaries within the field of NGC 188 (the orbit for blue straggler binary 7782 is shown in the Figure on the right). We are currently working on completing our analysis paper in which we determine the binary frequency and distributions of orbital parameters for the main sequence, giant and blue straggler cluster members. I am also leading the analysis of the binaries in M67 and M35, and working with my WOCS colleagues at the University of Wisconsin - Madison to examine the binaries in NGC 6819, NGC 7789 and NGC 2516.

In our upcoming NGC 188 binary analysis paper, we also compare the NGC 188 binaries to those from a recent N-body open cluster model (created by my collaborator Jarrod Hurley). We find that the standard assumptions used to define the initial binaries in such models result in mature binary populations that are significantly different than real binaries in true clusters like NGC 188. This finding motivated us to create a more realistic open cluster model, as discussed below, by defining the initial binaries directly from observations of young open clusters.

Indeed binary populations used in numerical simulations have long been based upon theoretical inferences and predictions. Yet the binary population dictates the dynamical evolution of the parent open cluster. Furthermore, the details of dynamical encounters are determined in a large part by the orbital parameters and masses of the binaries involved. Therefore accurately modeling the effects of dynamical encounters on stellar (and planetary) systems in star clusters requires an accurate initial binary population. A robust empirical definition of the initial stellar population can only be achieved through the study of young open clusters (ages <500 Myr), such as M35, M37, NGC 3532 and NGC 2516.

Collaborators: Bob Mathieu, Natalie Gosnell, Katelyn Milliman, Søren Meibom, David Latham, Sydney Barnes, David James, Keivan Stassun, Hugh Harris

Papers: Geller et al. (2009, 2011), Stassun et al.(2008)

Press: For Stassun et al. (2008):


Student Projects: Our observations of M37, NGC 3532 and NGC 2516 are at the perfect stage for the first analysis of the binary population. Students can develop methods to detect the binaries in the cluster, given a time series of radial velocities for a population of stars (hint: start with calculating the respective standard deviations of the radial velocities for each star). Once the binaries are detected, we will prioritize them in our upcoming observing runs to be sure that we can obtain enough measurements to determine their kinematic orbital solutions (like the Figure to the right). Given identified binaries, students can be the first to calculate the binary frequency, and given sufficient binary orbits, students can be the first to determine the distributions of period, eccentricity, etc., all of which are critical ingredients for creating N-body open cluster models.

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Exotic Stars
Blue Straggler Creation Through Mass Transfer My artistic representation of a blue straggler being created by mass transfer in a binary star system. The giant star, seen in the upper left of the illustration, has lost hold of its outer envelope. This material is pulled towards its partner, forming an accretion disk, and is eventually consumed by the "proto-blue straggler", seen in the lower right of the illustration. Soon the giant star will donate the remainder of its envelope, leaving only the half-solar-mass white dwarf core (shown peaking through the giant's tenuous envelope) as the companion to the blue straggler.
Credit: A. M. Geller
Blue Straggler CMD
Brightness (increasing upwards) in V magnitudes versus color (redder and cooler to the right) in B-V magnitudes. The 21 blue stragglers are shown as larger black dots, with the 16 binaries circled (and the two double-lined binaries marked with 2 concentric circles), and are identified as being to the left of the dashed line at a given brightness. The line is drawn so as to not include binaries comprising two normal stars from the cluster turn-off region, which consequently are brighter in combination. For reference, we also show a zero-age main sequence (solid line). Normal single stars spend most of their main-sequence lives very near this line until their core hydrogen supply is exhausted and they evolve towards the giant branch.
Credit: R. D. Mathieu & A. M. Geller (2009, Nature)

Recently, through careful cluster membership analyses, we have found rich populations of exotic stars. These stars are not predicted by stellar evolution theory and instead derive from stellar collisions, mergers, mass transfer and dynamical encounters, many of which are facilitated by binary stars. The "blue stragglers" are the most well studied example, and are generally identified by their unique location on the color-magnitude diagram, being hotter and brighter than the main sequence turnoff stars. Other exotic stars can be identified by rapid rotation (which is easily detected in our spectroscopic data), X-ray emission (e.g., in our XMM-Newton observations), and also through unlikely binary orbits.

Lately, I have been particularly interested in blue stragglers. Blue stragglers are stars observed to be brighter and bluer than normal main sequence stars of a similar mass and age, and therefore long ago should have evolved to become giant stars and stellar remnants. Since the discovery of blue stragglers, some 60 years ago in the globular cluster M3 by Allan Sandage, blue stragglers have been observed in essentially every stellar population where astronomers have looked, from the very dense cores of globular clusters, to the moderately dense open star clusters, to the sparse regions of the Galactic field. Astronomers have been debating the origins of blue stragglers within these various environments since their discovery. The currently accepted theories include formation through collisions, mergers and mass transfer.

Stellar collisions can occur in the dense regions of star clusters when two stars physically run into each other, and combine to form one more massive star, that would then be observed as a blue straggler. It is most likely that such collisions would occur as a result of dynamical encounters involving binary stars, given their larger physical cross sections for interactions. Therefore a blue straggler created in a collision may retain a companion that participated in the encounter.

Mergers are similar to collisions in that two stars come together to form one blue straggler. However in this scenario the stars begin bound in a close binary system. In fact, the two stars are so close that, given an angular momentum loss mechanism (like magnetic braking), the two stars eventually touch and spiral in to merge. This particular scenario would produce a single blue straggler. Recently this mechanism has been discussed in the context of a triple star system where Kozai cycles drive the inner binary to high eccentricity, and tidal dissipation during close pericenter passages shrinks the orbit to induce a merger. In this new scenario, the original tertiary star would remain bound to the blue straggler as a binary companion.

Mass transfer also occurs within a binary system, but in this scenario the stars do not merge. Instead one star evolves to become a giant and then overfills its Roche Lobe. The giant transfers mass from its envelope to the main sequence star, which accretes the material and eventually becomes a blue straggler. Once the giant has donated its entire envelope, all that remains as a companion to the blue straggler is a white dwarf (the remnant core of the giant star donor), which is predicted to be about 0.5 solar masses. This scenario is shown in my illustration to the right.

Along with my collaborator Bob Mathieu from the University of Wisconsin - Madison, I tested these formation hypotheses against our observations of the blue stragglers in the old (7 Gyr) open cluster NGC 188. The NGC 188 blue stragglers have a remarkably high binary frequency, and nearly all of the companions to the blue stragglers orbit with periods near 1000 days. Importantly, we also find that these long-period blue straggler binaries in NGC 188 all have companions of about half a solar mass.

Through comparisons of these detailed observations to blue stragglers created within our sophisticated N-body model of NGC 188, we conclusively rule out an origin in collisions for these long-period blue straggler binaries. Blue stragglers formed by collisions, which remain in binaries, have significantly higher-mass companions and significantly higher eccentricities than are observed. Mergers in hierarchical triples are marginally permitted by the observations, but the data do not favor this hypothesis. Instead the data are closely consistent with a mass transfer origin for the long-period blue straggler binaries in NGC 188, in which the companions would be half-solar-mass white dwarfs.

This is the first time that the origins of nearly every blue straggler in a star cluster have been determined, and the mass transfer mechanism has emerged as a compelling candidate. We aim to confirm this result through forthcoming Hubble Space Telescope observations which can directly detect the ultraviolet flux from the white dwarf companions predicted by the mass transfer mechanism.

Collaborators: Bob Mathieu, Natalie Gosnell, Katelyn Milliman, David Latham, Nathan Leigh, Alison Sills

Papers:Geller & Mathieu (2011), Mathieu & Geller (2009), Gosnell, et al. (2011)

Press: For Geller & Mathieu (2011):

For Mathieu & Geller (2009):


Student Projects: Students can perform the first census of exotic stars within M37, NGC 3532 and NGC 2516, which will undoubtedly include serendipitous discovers. Though blue stragglers in these clusters would be too bright to be included in our stellar samples, we can search for exotic stars that show anomalously high rotation rates, unexpected binary orbits, or possibly surprising X-ray emission (in my collaborators Chandra and XMM X-ray data for NGC 3532 and NGC2516). By investigating the origins of these stars you can form exciting and rewarding research projects. Indeed the undergraduate theses of Tom Finzell, Matthew Bailey and Mike DiPompeo, all of whom I co-mentored, were based, in part, on similar studies.

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N-body Open Cluster Simulations
N-body snapshotVisualization showing a snapshot in time from an N-body open cluster simulation. The simulation was created using the nbody6 code, and this image was created using my personal visualization software.
Credit: A. M. Geller

N-body comparions to observationsComparison of the NGC 188 N-body model to our observations. The left panels compare the observed (black line) and simulated (gray-filled) main sequence period (top) and eccentricity (bottom) distributions. The right panel compares the simulated (left) and observed (right) color-magnitude diagrams (with the main-sequence binaries used for the left panels marked in gray). The initial binaries for the NGC 188 simulation were based directly on our observations of the binary population in the young (150 Myr) open cluster M35. The simulation was constructed using the nbody6 code. The remarkable agreement between the binary population in the model and that of the true cluster in both frequency and distributions of orbital parameters demonstrates the power of using detailed observations to guide sophisticated N-body simulations.
Credit: A. M. Geller

N-body codes have matured over nearly the past half a decade under careful development by Dr. Sverre Aarseth and collaborators, and now the interaction between stellar evolution and dynamics can be modeled self-consistently (e.g. nbody6). The groundbreaking Hurley et al. (2005) open cluster model (discussed briefly above) is a clear example of the potential for such numerical studies to address long-standing questions about binary evolution and the origins of blue stragglers in a specific open cluster. However upon a more detailed comparison of this model to our data, it became clear that critical discrepancies remained, especially in the binary population.

During the 2009 summer, I was awarded an NSF EAPSI fellowship to work with Dr. Jarrod Hurley at the Swinburne Centre for Astrophysics and Supercomputing to create an accurate N-body model of the old (7 Gyr) open cluster NGC 188. Our innovation was to use our observations of the binary population in the young (150 Myr) open cluster M35 to directly establish the initial binary population in the simulation, thereby replacing the theoretical distributions that have long been used in the absence of detailed observations. The NGC 188 model is the first simulation whose primordial binaries are directly defined by such detailed observations of a young open cluster.

There is no a priori reason to assume that M35 and NGC 188 are on the same evolutionary sequence. Still, at 7 Gyr the simulation matches the observed main sequence binary period and eccentricity distributions and binary frequency with remarkable accuracy, a vast improvement over previous N-body models. The excellent agreement between our model and our detailed observations of the true cluster demonstrates the power of using observations of real binary populations to directly define the initial conditions of open cluster N-body models. Furthermore, the accuracy with which we reproduce the normal binaries in the cluster allowed us to finally investigate the origins of the NGC 188 blue stragglers within a realistic and comprehensive theoretical framework (discussed above).

Collaborators: Jarrod Hurley, Bob Mathieu

Papers: Geller et al. (2008), Geller, Hurley & Mathieu (2009), Geller & Mathieu (2011), and "A Direct N-body Model of the Old Open Cluster NGC 188, Geller, Hurley & Mathieu in prep

Press: For Geller & Mathieu (2011):


Student Projects: A single N-body open cluster simulation can form the basis of numerous student projects. Analyses of our NGC 188 N-body model have proven extremely rewarding, and we have yet to study even half of the available projects, which range from comparing the simulated binaries with the observed binary population in the true cluster, to determining the origins of exotic stars, to identifying and addressing areas within the code that need improvement in order to match observations. Moreover, there are numerous established projects available to students within this completed N-body model. Additionally students can create and analyze their own N-body simulation(s) (potentially based on the observations of M37, NGC 2516 and NGC 3532 discussed previously). One particularly compelling project is the investigation of how dynamical encounters effect planetary systems within star clusters, which can readily be studied within an N-body open cluster model.

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Exoplanets in Star Clusters
Solar System EncounterSemi-major axes as functions of time for the planets in our Solar System, produced using the Mercury planetary system integrator. The gray lines show the normal unperturbed system, and the black lines show what our Solar System would look like in the 200 years following a weak dynamical encounter with another star, for instance within an open star cluster. Neptune, Uranus and Saturn are ejected from the system. The rest of the planets survive, but their semi-major axes (as well as eccentricities, and inclinations) are modified, with Jupiter's orbit changed most significantly. I will use as similar method to model the dynamical evolution, including the effects of stellar encounters, of planetary systems within star clusters.
Credit: A. M. Geller

A large fraction of stars form in star clusters or cluster-like environments. Indeed many stars found in the field today were likely born in denser environments, and were therefore subject to dynamical encounters with other stars in the past. Such dynamical interactions can reshape a population of planetary systems by modifying their orbits and can potentially lead to their disruption. Furthermore even small perturbations to multiple-planet systems (e.g. those inducing modest changes in eccentricity or inclination) can have catastrophic effects on the system's internal evolution, possibly leading to collisions, ejected planets or the complete disruption of the system. It is therefore remarkable that 34% of observed stars in the Kepler field host at least one planet (a < 0.5 AU), and a third of the planetary systems contain multiple planets.

Though observational surveys of open clusters are not yet ready to answer the question of how the dynamical environment of a star cluster can effect planetary systems (due to small samples and selection biases), N-body simulations can do so today. Furthermore, we can now use our observations of the stellar populations in open clusters, to guide sophisticated star cluster models with greater accuracy than was previously possible.

Soon, I will create an array of N-body open cluster simulation spanning the observed masses and densities for open cluster in our Galaxy, to study how stellar encounters within star clusters effect the dynamical evolution of planetary systems (including those similar to our Solar System). Within these simulations we will track the evolution of planetary systems containing multiple planets to answer the following fundamental questions:

  1. What fraction of planetary systems can survive in open cluster environments of different masses,densities and ages, and what are their orbital parameters?
  2. What fraction of the surviving planets are in the habitable regions around their host stars?
  3. How are the orbital parameters of surviving planetary systems modified by dynamical encounters, and does this vary significantly for different mass host stars?
  4. What insights do our simulations provide for results from recent observational exoplanet searches in open clusters, and what predictions do our simulations make for future surveys?
  5. What are the characteristics of planetary systems that escape from clusters, and do they show detectable signatures of dynamical encounters?

Collaborators: Simon Portegies Zwart, Inti Pelupessy, Jarrod Hurley, Fred Rasio, Yoram Lithwick, Daniel Fabrycky


Student Projects: I plan to create about 100 unique N-body models, which will include in total about 200,000 single stars hosting planetary systems. I could really use your help to run, monitor and analyze these simulations! We'll need to develop automated analysis software, and a talented student can help to develop these tools. Alternatively, you can take ownership over one (or more) of these N-body models to investigate any myriad of research directions of your choosing. This is an exciting project that we will begin soon, and you have the opportunity to get in on the "ground floor"!

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Three-Body Evolution

My collaborators and I are developing the first code that models both the secular dynamics and stellar evolutionary processes of three-body systems. Triple stars have been employed to explain the production of a number of exotic star systems, including certain X-ray binaries, blue stragglers, contact binaries and type Ia supernovae progenitors. With our, we will test these hypotheses in full detail. Dynamical interactions in two-planet systems have been postulated to explain observed retrograde planets and "hot Jupiters". We will use our code to explore the effects of stellar evolutionary process on these mechanisms. Additionally, we will study the stability of a planet orbiting an evolving binary star, which is particularly exciting given the first circumbinary planet recently discovered by Kepler.

We are currently in the development stages of this code, and expect to have the code completed by early 2012.

Collaborators: Smadar Naoz, Hagai Perets, Paul Kiel


Student Projects: Interested and talented students can help us complete and improve the code, which is quite close, but requires a lot of testing to verify that we have captured all of the necessary physics. Once completed, students can use our code to test the formation hypotheses of the exotic star systems and unusual planetary systems mentioned above. This will be the first time that these theories have been tested in full detail, and will be very exciting projects!

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Contact Information (jointly appointed):
Northwestern University -- CIERA
2145 Sheridan Road, Evanston, IL 60208-3112, USA
Office: F233 Tech
Phone: (847) 467-5076   |   Fax: (847) 467-0679
Email: a-geller [at] northwestern.edu
The Adler Planetarium
Department of Astronomy
Museum Campus, 1300 S Lake Shore Dr, Chicago, IL 60605, USA
Phone: (312) 542-2410
Email: ageller [at] adlerplanetarium.org