@article{noauthororeditor,
  abstract = {Due to the wide deployment of sensitive information on the internet, privacy preserving data mining has been studied extensively in recent years. The emerging privacy concern has become a major obstacle in storing and sharing of medical data. The proliferation of medical data can be highly useful, but it must be performed in a way that preserves patient's privacy. This is not straightforward, because the proliferated data need to be protected against several privacy threats. Various algorithms have been designed for privacy-preserving data mining that can be classified into three categories i.e., privacy by policy, privacy by statistics, and privacy by cryptography, however, the privacy concerns and data utilization requirements on different parts of medical data may be quite different. In this paper, we present a survey of the state-of-the-art algorithms that have been proposed for publishing medical data in a privacy preserving way. We review algorithms like  Randomization, k-anonymization, and distributed privacy-preserving data mining etc., derive insights on their operation, and highlight their advantages and disadvantages. We also provide discussion of the computational and hypothetical boundaries associated with privacy-preservation over high dimensional data sets. Musavir Hassan | Muheet Ahmed Butt | Majid Zaman"Privacy Preserving Data Mining for Healthcare Record: A Survey of Algorithms" Published in International Journal of Trend in Scientific Research and Development (ijtsrd), ISSN: 2456-6470, Volume-2 | Issue-1 , December 2017, URL: http://www.ijtsrd.com/papers/ijtsrd7191.pdf  http://www.ijtsrd.com/computer-science/data-miining/7191/privacy-preserving-data-mining-for-healthcare-record-a-survey-of-algorithms/musavir-hassan
},
  added-at = {2018-09-01T14:28:43.000+0200},
  author = {Zaman, Musavir Hassan Muheet Ahmed Butt Majid},
  biburl = {https://www.bibsonomy.org/bibtex/2422b7d33af9e60a44b7c228812da0441/ijtsrd},
  interhash = {ce9a89ddd060c23752faf54147fc75e5},
  intrahash = {422b7d33af9e60a44b7c228812da0441},
  issn = {2456-6470},
  journal = {International Journal of Trend in Scientific Research and Development},
  keywords = {(Computer-based (EHRs) (Electronic (Privacy CPR Data Distributed EMR Medical Miining PPD PPDDM Patient Record) Record). and electronic health mining) preserving records},
  language = {English},
  month = dec,
  number = 1,
  pages = {1176-1184},
  timestamp = {2018-10-02T11:01:27.000+0200},
  title = {Privacy Preserving Data Mining for Healthcare Record: A Survey of Algorithms
},
  url = {http://www.ijtsrd.com/computer-science/data-miining/7191/privacy-preserving-data-mining-for-healthcare-record-a-survey-of-algorithms/musavir-hassan},
  volume = 2,
  year = 2017
}

@inproceedings{cook2016using,
  abstract = {This paper proposes a methodology which attempts to address the barriers to the development of successful educational design research through a process which identifies gaps in current practices and devises innovations to target them. Educational design research assumes an ambitious position: a dual commitment to understand and contribute to both theory and practice. This task is confounded by the complexity of the domain and the inherent multi-stakeholder nature of most initiatives. Three barriers to success are identified: the shortage of mechanisms for cross-stakeholder dialogue, the failure to account for existing practices and contexts, and the rigid processes dictated by the dynamics of research projects. We report findings from an attempt to address these barriers. Confer is a Groupware tool that provides support to bridge face2face and online discussions by workgroups and has been co-designed with users by following the Participatory Patterns Design (PPD) methodology. The PPD provides a framework for engaging multidisciplinary communities in collaborative reflection on educational innovation in a given domain.},
  added-at = {2016-09-13T22:50:37.000+0200},
  address = {Vancouver, Canada},
  author = {Cook, John and Mor, Yishay and Santos, Patricia and Treasure-Jones, Tamsin and Elferink, Raymond and Kerr, Micky},
  biburl = {https://www.bibsonomy.org/bibtex/2e0cf561abbfcbf8a37f6b0ad0ce1d322/yish},
  booktitle = {EdMedia 2016},
  interhash = {d3c0a08330a2b607a6cd39b6406623fe},
  intrahash = {e0cf561abbfcbf8a37f6b0ad0ce1d322},
  keywords = {design inaglobe myown narratives patterns ppd ppw scenarios snap},
  month = {June},
  timestamp = {2022-11-20T15:18:38.000+0100},
  title = {Using the participatory patterns design (PPD) methodology to co-design groupware: Confer a tool for workplace informal learning},
  url = {http://eprints.uwe.ac.uk/27653/},
  year = 2016
}

@inproceedings{uweresearch27653,
  abstract = {This paper proposes a methodology which attempts to address the barriers to the development of successful educational design research through a process which identifies gaps in current practices and devises innovations to target them. Educational design research assumes an ambitious position: a dual commitment to understand and contribute to both theory and practice. This task is confounded by the complexity of the domain and the inherent multi-stakeholder nature of most initiatives. Three barriers to success are identified: the shortage of mechanisms for cross-stakeholder dialogue, the failure to account for existing practices and contexts, and the rigid processes dictated by the dynamics of research projects. We report findings from an attempt to address these barriers. Confer is a Groupware tool that provides support to bridge face2face and online discussions by workgroups and has been co-designed with users by following the Participatory Patterns Design (PPD) methodology. The PPD provides a framework for engaging multidisciplinary communities in collaborative reflection on educational innovation in a given domain.},
  added-at = {2016-05-04T18:35:15.000+0200},
  author = {Cook, John and Mor, Yishay and Santos, Patricia and Treasure-Jones, Tamsin and Elferink, Raymond and Kerr, Miki},
  biburl = {https://www.bibsonomy.org/bibtex/272906e5b8f20e027643f21d89a7e5b4b/yish},
  booktitle = {EdMedia 2016},
  interhash = {d3c0a08330a2b607a6cd39b6406623fe},
  intrahash = {72906e5b8f20e027643f21d89a7e5b4b},
  keywords = {ODAT design education hybrid learning myown patterns ppd principles},
  month = {June},
  timestamp = {2016-05-04T21:52:24.000+0200},
  title = {Using the participatory patterns design (PPD) methodology to co-design groupware: Confer a tool for workplace informal learning},
  url = {http://eprints.uwe.ac.uk/27653/},
  year = 2016
}

@misc{duffell2014migration,
  abstract = {Most standard descriptions of Type II migration state that massive,
gap-opening planets must migrate at the viscous drift rate. This is based on
the idea that the disk is separated into an inner and outer region and gas is
considered unable to cross the gap. In fact, gas easily crosses the gap on
horseshoe orbits, nullifying this necessary premise which would set the
migration rate. In this work, it is demonstrated using highly accurate
numerical calculations that the actual migration rate is dependent on disk and
planet parameters, and can be significantly larger or smaller than the viscous
drift rate. In the limiting case of a disk much more massive than the
secondary, the migration rate saturates to a constant which is sensitive to
disk parameters and is not necessarily of order viscous rate. In the opposite
limit of a low-mass disk, the migration rate decreases linearly with disk mass.
Steady-state solutions in the low disk mass limit show no pile-up outside the
secondary's orbit, and no corresponding drainage of the inner disk.},
  added-at = {2014-08-05T16:33:58.000+0200},
  author = {Duffell, Paul C. and Haiman, Zoltan and MacFadyen, Andrew I. and D'Orazio, Daniel J. and Farris, Brian D.},
  biburl = {https://www.bibsonomy.org/bibtex/20bcaa058186d9e950d1ab3e8df20735f/danielcarrera},
  description = {[1405.3711] The Migration of Gap-Opening Planets is not Locked to Viscous Disk Evolution},
  interhash = {d079507b35851cdeaafef6215c7f6623},
  intrahash = {0bcaa058186d9e950d1ab3e8df20735f},
  keywords = {2014 PPD a:Duffell a:Haiman gap giant planets},
  note = {cite arxiv:1405.3711Comment: ApJ Accepted},
  timestamp = {2014-08-05T16:33:58.000+0200},
  title = {The Migration of Gap-Opening Planets is not Locked to Viscous Disk
  Evolution},
  url = {http://arxiv.org/abs/1405.3711},
  year = 2014
}

@misc{tsukamoto2014effects,
  abstract = {We investigate structure of self-gravitating disks, their fragmentation and
evolution of the fragments (the clumps) using both analytic approach and
three-dimensional radiation hydrodynamics simulations. The simulations show
that non-local radiation transfer determines disk temperature. We find the disk
structure is well described by an analytical model of quasi-steady
self-gravitating disk. Because the radiation process is not local and radiation
from the interstellar medium cannot be ignored, the local balance between the
radiation cooling and the viscous heating is not achieved in a massive disk
around a low mass star. In our simulations, there are cases in which the disk
does not fragment even though it satisfies the fragmentation criterion based on
disk cooling time ($Q \sim 1$ and $\Omega t_{\rm cool}\sim 1$). This indicates
that at least the criterion is not sufficient condition for fragmentation. We
also investigate the disk fragmentation process induced by mass accretion from
the envelope. We determine the parameter range for the host cloud core in which
disk fragmentation occurs. In addition, we show that the temperature evolution
of the center of the clump is almost consistent with that of a typical first
core and we show the minimum initial mass of clumps to be about a few Jupiter
mass.},
  added-at = {2014-08-05T16:33:24.000+0200},
  author = {Tsukamoto, Yusuke and Takahashi, Sanemichi Z. and Machida, Masahiro N. and Inutsuka, Shu-ichiro},
  biburl = {https://www.bibsonomy.org/bibtex/2e1b09e7cdacf67af95e97fdbc386d702/danielcarrera},
  description = {[1404.7271] Effects of radiation transfer on the structure of self-gravitating disks, their fragmentation and evolution of the fragments},
  interhash = {ab5188c57294e42358bf7904c4a4b349},
  intrahash = {e1b09e7cdacf67af95e97fdbc386d702},
  keywords = {2014 PPD a:Tsukamoto a:takahashi radiative-transfer self-gravity},
  note = {cite arxiv:1404.7271Comment: 17 pages, 13 figures, submitted to MNRAS},
  timestamp = {2014-08-05T16:33:24.000+0200},
  title = {Effects of radiation transfer on the structure of self-gravitating
  disks, their fragmentation and evolution of the fragments},
  url = {http://arxiv.org/abs/1404.7271},
  year = 2014
}

@misc{kirchschlager2014effect,
  abstract = {We theoretically analyze protoplanetary disks consisting of porous dust
grains. In the analysis of observations of protoplanetary disks the dust phase
is often assumed to consist of spherical grains, allowing one to apply the Mie
scattering formalism. However, in reality, the shape of dust grains is expected
to deviate strongly from that of a sphere. We investigate the influence of
porous dust grains on the temperature distribution and observable appearance of
protoplanetary disks for dust grain porosities of up to 60 %. We performed
radiative transfer modeling to simulate the temperature distribution, spectral
energy distribution, and spatially resolved intensity and polarization maps.
The optical properties of porous grains were calculated using the method of
discrete dipole approximation. We find that the flux in the optical wavelength
range is for porous grains higher than for compact, spherical grains. The
profile of the silicate peak at 9.7 um strongly depends on the degree of grain
porosity. The temperature distribution shows significant changes in the
direction perpendicular to the midplane. Moreover, simulated polarization maps
reveal an increase of the polarization degree by a factor of about four when
porous grains are considered, regardless of the disk inclination. The
polarization direction is reversed in selected disk regions, depending on the
wavelength, grain porosity, and disk inclination. We discuss several possible
explanations of this effect and find that multiple scattering explains the
effect best. Porosity influences the observable appearance of protoplanetary
disks. In particular, the polarization reversal shows a dependence on grain
porosity. The physical conditions within the disk are altered by porosity,
which might have an effect on the processes of grain growth and disk evolution.},
  added-at = {2014-07-25T17:15:04.000+0200},
  author = {Kirchschlager, F. and Wolf, S.},
  biburl = {https://www.bibsonomy.org/bibtex/22c8ae0c6435bb72e76d9feca8f3ada30/danielcarrera},
  description = {[1407.6575] Effect of dust grain porosity on the appearance of protoplanetary disks},
  interhash = {b1e5cd71b0cd18e59f01d0cc89ed8e8a},
  intrahash = {2c8ae0c6435bb72e76d9feca8f3ada30},
  keywords = {2014 PPD a:Kirchschlager a:Wolf dust observations},
  note = {cite arxiv:1407.6575Comment: 12 pages, 18 figures},
  timestamp = {2014-07-25T17:15:04.000+0200},
  title = {Effect of dust grain porosity on the appearance of protoplanetary disks},
  url = {http://arxiv.org/abs/1407.6575},
  year = 2014
}

@misc{raymond2014universal,
  abstract = {It has been proposed that the observed systems of hot super-Earths formed in
situ from high-mass disks. By fitting a disk profile to the entire population
of Kepler planet candidates, Chiang & Laughlin (2013) constructed a
"minimum-mass extrasolar nebula" with surface density profile Sigma r^-1.6.
Here we use multiple-planet systems to show that it is inconsistent to assume a
universal disk profile. Systems with 3-6 low-mass planets (or planet
candidates) produce a diversity of minimum-mass disks with surface density
profiles ranging from Sigma r^-3.2 to Sigma r^0.5 (5th-95th percentile). By
simulating the transit detection of populations of synthetic planetary systems
designed to match the properties of observed super-Earth systems, we show that
a universal disk profile is statistically excluded at high confidence. Rather,
the underlying distribution of minimum-mass disks is characterized by a broad
range of surface density slopes. Models of gaseous disks can only explain a
narrow range of slopes (roughly between r^0 and r^-1.5). Yet accretion of
terrestrial planets in a gas-free environment preserves the initial radial
distribution of building blocks. The known systems of hot super-Earths must
therefore not represent the structure of their parent gas disks and can not
have predominantly formed in situ. We instead interpret the diversity of disk
slopes as the imprint of a process that re-arranged the solids relative to the
gas in the inner parts of protoplanetary disks. A plausible mechanism is inward
type 1 migration of Mars- to Earth-mass planetary embryos, perhaps followed by
a final assembly phase.},
  added-at = {2014-02-04T11:35:20.000+0100},
  author = {Raymond, Sean N. and Cossou, Christophe},
  biburl = {https://www.bibsonomy.org/bibtex/274539653a24f30c3a5d57d68ee01068f/danielcarrera},
  description = {[1401.3743] No universal minimum-mass extrasolar nebula: Evidence against in-situ accretion of systems of hot super-Earths},
  interhash = {ad9e2dac4a94a7488d512aa69748f375},
  intrahash = {74539653a24f30c3a5d57d68ee01068f},
  keywords = {2014 MMEN MMSN PPD a:Cossou a:Raymond formation planets},
  note = {cite arxiv:1401.3743Comment: Accepted to MNRAS Letters. 5 pages, 3 figures. (Updated references)},
  timestamp = {2014-07-25T17:15:16.000+0200},
  title = {No universal minimum-mass extrasolar nebula: Evidence against in-situ
  accretion of systems of hot super-Earths},
  url = {http://arxiv.org/abs/1401.3743},
  year = 2014
}

@misc{chiang2012minimummass,
  abstract = {Close-in super-Earths, with radii R = 2-5 R_Earth and orbital periods P < 100
days, orbit more than half, and perhaps nearly all Sun-like stars in the
universe. We use this omnipresent population to construct the minimum-mass
extrasolar nebula (MMEN), the circumstellar disk of solar-composition solids
and gas from which such planets formed, if they formed near their current
locations and did not migrate. In a series of back-of-the-envelope
calculations, we demonstrate how in-situ formation in the MMEN is fast,
efficient, and can reproduce many of the observed properties of close-in
super-Earths, including their gas-to-rock fractions. Testable predictions are
discussed.},
  added-at = {2014-02-03T12:56:07.000+0100},
  author = {Chiang, E. and Laughlin, G.},
  biburl = {https://www.bibsonomy.org/bibtex/2aa4e4e5e6de6e554d3d4dd9d396f0a3a/danielcarrera},
  description = {[1211.1673] The Minimum-Mass Extrasolar Nebula: In-Situ Formation of Close-In Super-Earths},
  interhash = {4a826370ec85cf4af268d1d84cb953e2},
  intrahash = {aa4e4e5e6de6e554d3d4dd9d396f0a3a},
  keywords = {2012 MMEN MMSN PPD a:Chiang a:Laughlin formation planets super-earth},
  note = {cite arxiv:1211.1673Comment: Accepted to MNRAS 2013 March 6},
  timestamp = {2014-07-25T17:15:21.000+0200},
  title = {The Minimum-Mass Extrasolar Nebula: In-Situ Formation of Close-In
  Super-Earths},
  url = {http://arxiv.org/abs/1211.1673},
  year = 2012
}

@misc{podlewskagaca2013presence,
  abstract = {In this paper we investigate the possibility of a migration-induced resonance
locking in systems containing three planets, namely an Earth analog, a
super-Earth and a gas giant. The planets have been listed in order of
increasing orbital periods. All three bodies are embedded in a locally
isothermal gaseous disc and orbit around a solar mass star. We are interested
in answering the following question: Will the low-mass planets form the same
resonant structures with each other in the vicinity of the gas giant as in the
case when the gas giant is absent? When there is no gas giant in the system, it
has been already shown that if the two low-mass planets undergo a convergent
differential migration, they will capture each other in a mean-motion
resonance. For the choices of disc parameters and planet masses made in this
paper, the formation of the 5:4 resonance in the absence of the Jupiter has
been observed. In this work we add a gas giant on the most external orbit of
the system in such a way that its differential migration is convergent with the
low-mass planets. We show that the result of this set-up is the speeding up of
the migration of the super-Earth and, after that, all three planets become
locked in a triple mean-motion resonance. However, this resonance is not
maintained due to the low-mass planet eccentricity excitation, a fact that
leads to close encounters between planets and eventually to the ejection from
the internal orbits of one or both low-mass planets.},
  added-at = {2013-12-13T16:52:25.000+0100},
  author = {Podlewska-Gaca, Edyta and Szuszkiewicz, Ewa},
  biburl = {https://www.bibsonomy.org/bibtex/2b559d30049fdc8bc1e992df497a26dcb/danielcarrera},
  description = {[1312.2147] How the presence of a gas giant affects the formation of mean-motion resonances between two low-mass planets in a locally isothermal gaseous disc},
  interhash = {44c05741e28f8cdfd5dbb66f56fd9a2a},
  intrahash = {b559d30049fdc8bc1e992df497a26dcb},
  keywords = {2013 MMR PPD formation planets resonance},
  note = {cite arxiv:1312.2147Comment: 10 pages, 11 figures, to be published in MNRAS},
  timestamp = {2013-12-13T16:52:25.000+0100},
  title = {How the presence of a gas giant affects the formation of mean-motion
  resonances between two low-mass planets in a locally isothermal gaseous disc},
  url = {http://arxiv.org/abs/1312.2147},
  year = 2013
}

@article{1974MNRAS.168..603L,
  added-at = {2013-09-23T09:45:37.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/1974MNRAS.168..603L},
  author = {{Lynden-Bell}, D. and {Pringle}, J. E.},
  biburl = {https://www.bibsonomy.org/bibtex/2e3f1d2e3b4bc37f6d2877d70b8252c7f/danielcarrera},
  description = {The evolution of viscous discs and the origin of the nebular variables.},
  interhash = {1c0730d906a2dc178049295176f69b1a},
  intrahash = {e3f1d2e3b4bc37f6d2877d70b8252c7f},
  journal = {\mnras},
  keywords = {1974 PPD a:Lynden-Bell a:Pringle formation key planets},
  month = sep,
  pages = {603-637},
  timestamp = {2014-07-25T17:15:35.000+0200},
  title = {{The evolution of viscous discs and the origin of the nebular variables.}},
  volume = 168,
  year = 1974
}

@misc{meru2013large,
  abstract = {We perform coagulation & fragmentation simulations to understand grain growth
in T Tauri & brown dwarf discs. We present a physically-motivated approach
using a probability distribution function for the collision velocities and
separating the deterministic & stochastic velocities. We find growth to larger
sizes compared to other models. Furthermore, if brown dwarf discs are
scaled-down versions of T Tauri discs (in terms of stellar & disc mass, and
disc radius), growth at the same location with respect to the outer edge occurs
to similar sizes in both discs.},
  added-at = {2013-08-26T09:51:59.000+0200},
  author = {Meru, Farzana and Galvagni, Marina and Olczak, Christoph and Garaud, Pascale},
  biburl = {https://www.bibsonomy.org/bibtex/2f6fd59b369824c625e8fab5e719afc3b/danielcarrera},
  description = {[1308.5181] Large grains can grow in circumstellar discs},
  interhash = {7cccab11f6e86e8a42869f32b8a73859},
  intrahash = {f6fd59b369824c625e8fab5e719afc3b},
  keywords = {2013 PPD coagulation formation planets},
  note = {cite arxiv:1308.5181Comment: Submitted to the conference proceedings of the IAU Symposium 299 -  Exploring the formation and evolution of planetary systems. 2 pages; 2  figures},
  timestamp = {2014-07-25T17:15:44.000+0200},
  title = {Large grains can grow in circumstellar discs},
  url = {http://arxiv.org/abs/1308.5181},
  year = 2013
}

@article{2013arXiv1308.1791A,
  added-at = {2013-08-09T14:07:07.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2013arXiv1308.1791A},
  archiveprefix = {arXiv},
  author = {{Alexander}, R.},
  biburl = {https://www.bibsonomy.org/bibtex/23df7f262c247b522815a237306c5a30c/danielcarrera},
  description = {Planet formation in evolving protoplanetary discs},
  eprint = {1308.1791},
  interhash = {00d8f6218fcb5b9d1b631b28f83c2067},
  intrahash = {3df7f262c247b522815a237306c5a30c},
  journal = {ArXiv e-prints},
  keywords = {2013 PPD a:aAlexander formation planets review},
  month = aug,
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:15:49.000+0200},
  title = {{Planet formation in evolving protoplanetary discs}},
  url = {http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1308.1791},
  year = 2013
}

@article{2012A&A...538A.114P,
  added-at = {2013-08-05T15:20:16.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2012A%26A...538A.114P},
  archiveprefix = {arXiv},
  author = {{Pinilla}, P. and {Birnstiel}, T. and {Ricci}, L. and {Dullemond}, C. P. and {Uribe}, A. L. and {Testi}, L. and {Natta}, A.},
  biburl = {https://www.bibsonomy.org/bibtex/20f8db43dcd33b661705811c93e8f6201/danielcarrera},
  description = {Trapping dust particles in the outer regions of protoplanetary disks},
  doi = {10.1051/0004-6361/201118204},
  eid = {A114},
  eprint = {1112.2349},
  interhash = {bf87fad8000700acd6245e451c9d464f},
  intrahash = {0f8db43dcd33b661705811c93e8f6201},
  journal = {\aap},
  keywords = {2012 PPD a:Dullemond a:Pinilla a:Testi dust formation numerical planets},
  month = feb,
  pages = {A114},
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:20:10.000+0200},
  title = {{Trapping dust particles in the outer regions of protoplanetary disks}},
  url = {http://adsabs.harvard.edu/abs/2012A%26A...538A.114P},
  volume = 538,
  year = 2012
}

@article{2013arXiv1301.2600H,
  added-at = {2013-08-05T02:21:58.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2013arXiv1301.2600H},
  archiveprefix = {arXiv},
  author = {{Hopkins}, P. F. and {Christiansen}, J. L.},
  biburl = {https://www.bibsonomy.org/bibtex/221b8781e2b367e9e742a2aecd0925416/danielcarrera},
  description = {Turbulent Disks are Never Stable: Fragmentation and Turbulence-Promoted Planet F},
  eprint = {1301.2600},
  interhash = {3ff8797f904ed9194078d7a8028aa7c6},
  intrahash = {21b8781e2b367e9e742a2aecd0925416},
  journal = {ArXiv e-prints},
  keywords = {2013 PPD a:Hopkins formation planets turbulence},
  month = jan,
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:16:15.000+0200},
  title = {{Turbulent Disks are Never Stable: Fragmentation and Turbulence-Promoted Planet Formation}},
  url = {http://adsabs.harvard.edu/abs/2013arXiv1301.2600H},
  year = 2013
}

@article{2007ApJ...662..627J,
  added-at = {2013-08-05T02:15:36.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...662..627J},
  author = {{Johansen}, A. and {Youdin}, A.},
  biburl = {https://www.bibsonomy.org/bibtex/2959f9b089ede0ec870c24a4fda203630/danielcarrera},
  description = {Protoplanetary Disk Turbulence Driven by the Streaming Instability: Nonlinear Sa},
  doi = {10.1086/516730},
  eprint = {arXiv:astro-ph/0702626},
  interhash = {23fe2698c0ee3d6eca3255123d050fb5},
  intrahash = {959f9b089ede0ec870c24a4fda203630},
  journal = {\apj},
  keywords = {2007 PPD a:Johansen a:Youdin numerical planets streaming-instability turbulence},
  month = jun,
  pages = {627-641},
  timestamp = {2014-07-25T17:16:24.000+0200},
  title = {{Protoplanetary Disk Turbulence Driven by the Streaming Instability: Nonlinear Saturation and Particle Concentration}},
  url = {http://adsabs.harvard.edu/abs/2007ApJ...662..627J},
  volume = 662,
  year = 2007
}

@article{2007A&A...462..977K,
  added-at = {2013-08-05T02:11:36.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2007A%26A...462..977K},
  author = {{Krauss}, O. and {Wurm}, G. and {Mousis}, O. and {Petit}, J.-M. and {Horner}, J. and {Alibert}, Y.},
  biburl = {https://www.bibsonomy.org/bibtex/21052727bafc7f51a867921f37e9b2c3d/danielcarrera},
  description = {The photophoretic sweeping of dust in transient protoplanetary disks},
  doi = {10.1051/0004-6361:20066363},
  eprint = {arXiv:astro-ph/0611757},
  interhash = {ef1afff78721e2ecd4379deb83b7cc7e},
  intrahash = {1052727bafc7f51a867921f37e9b2c3d},
  journal = {\aap},
  keywords = {2007 PPD dust planets transient},
  month = feb,
  pages = {977-987},
  timestamp = {2014-07-25T17:16:27.000+0200},
  title = {{The photophoretic sweeping of dust in transient protoplanetary disks}},
  url = {http://adsabs.harvard.edu/abs/2007A%26A...462..977K},
  volume = 462,
  year = 2007
}

@article{2009arXiv0905.4404I,
  added-at = {2013-08-04T21:59:14.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2009arXiv0905.4404I},
  archiveprefix = {arXiv},
  author = {{Ishitsu}, N. and {Inutsuka}, S.-i. and {Sekiya}, M.},
  biburl = {https://www.bibsonomy.org/bibtex/28e6d1d157af7819163a0377c5e9d0846/danielcarrera},
  description = {Two-fluid Instability of Dust and Gas in the Dust Layer of a Protoplanetary Disk},
  eprint = {0905.4404},
  interhash = {e7a40cdc59fca60cb4e118005107d944},
  intrahash = {8e6d1d157af7819163a0377c5e9d0846},
  journal = {ArXiv e-prints},
  keywords = {2009 PPD dust hydrodynamics numerical planets},
  month = may,
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:16:31.000+0200},
  title = {{Two-fluid Instability of Dust and Gas in the Dust Layer of a Protoplanetary Disk}},
  url = {http://adsabs.harvard.edu/abs/2009arXiv0905.4404I},
  year = 2009
}

@article{2013ApJ...764..194B,
  added-at = {2013-08-04T20:53:48.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2013ApJ...764..194B},
  archiveprefix = {arXiv},
  author = {{Boss}, A. P.},
  biburl = {https://www.bibsonomy.org/bibtex/2bf2243ea2bb92e356b801c256dd58639/danielcarrera},
  description = {Orbital Migration of Protoplanets in a Marginally Gravitationally Unstable Disk},
  doi = {10.1088/0004-637X/764/2/194},
  eid = {194},
  eprint = {1301.3178},
  interhash = {f2e847cd64dfb65791b3354f3ae49a13},
  intrahash = {bf2243ea2bb92e356b801c256dd58639},
  journal = {\apj},
  keywords = {2013 PPD disks gravitational-instability migration planets},
  month = feb,
  pages = 194,
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:16:45.000+0200},
  title = {{Orbital Migration of Protoplanets in a Marginally Gravitationally Unstable Disk}},
  url = {http://adsabs.harvard.edu/abs/2013ApJ...764..194B},
  volume = 764,
  year = 2013
}

@article{2013ApJ...772...75J,
  added-at = {2013-08-04T20:49:39.000+0200},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System},
  adsurl = {http://adsabs.harvard.edu/abs/2013ApJ...772...75J},
  archiveprefix = {arXiv},
  author = {{Jalali}, M. A.},
  biburl = {https://www.bibsonomy.org/bibtex/2e2716f9bd01379694ce9e06f4b77f9ed/danielcarrera},
  description = {Global Drag-induced Instabilities in Protoplanetary Disks},
  doi = {10.1088/0004-637X/772/1/75},
  eid = {75},
  eprint = {1301.2064},
  interhash = {3679819c91f250fbb4a4e1301abe58d1},
  intrahash = {e2716f9bd01379694ce9e06f4b77f9ed},
  journal = {\apj},
  keywords = {2013 PPD hydrodynamics numerical planets streaming-instability},
  month = jul,
  pages = 75,
  primaryclass = {astro-ph.EP},
  timestamp = {2014-07-25T17:16:58.000+0200},
  title = {{Global Drag-induced Instabilities in Protoplanetary Disks}},
  url = {http://adsabs.harvard.edu/abs/2013ApJ...772...75J},
  volume = 772,
  year = 2013
}

@incollection{Williams2011,
  abstract = {Flattened, rotating disks of cool dust and gas extending for tens to hundreds of AU are found around almost all low mass stars shortly after their birth. These disks generally persist for several Myr, during which time some material accretes onto the star, some is lost through outflows and photoevaporation, and some condenses into centimeter- and larger-sized bodies or planetesimals. Through observations mainly at infrared through millimeter wavelengths, we can determine how common disks are at different ages, measure basic properties including mass, size, structure, and composition, and follow their varied evolutionary pathways. In this way, we see the first steps toward exoplanet formation and learn about the origins of the Solar System. This review addresses observations of the outer parts, beyond 1 AU, of protoplanetary disks with a focus on recent infrared and (sub-)millimeter results and an eye to the promise of new facilities in the immediate future.},
  added-at = {2013-08-04T12:36:29.000+0200},
  archiveprefix = {arXiv},
  arxivid = {1103.0556},
  author = {Williams, Jonathan P and Cieza, Lucas A},
  biburl = {https://www.bibsonomy.org/bibtex/2e3c6e1842e86a375d5cd7386dd89e415/danielcarrera},
  booktitle = {Protoplanetary Disks},
  doi = {10.1146/annurev-astro-081710-102548},
  eprint = {1103.0556},
  file = {:home/daniel/Papers/Planets-PPDs/1108.AstroPh - Jonathan - Protoplanetary Disks and Their Evolution.pdf:pdf},
  interhash = {249f556d52be81fc6d651def2d4b6a66},
  intrahash = {e3c6e1842e86a375d5cd7386dd89e415},
  keywords = {2011 PPD accretion disks planets},
  mendeley-tags = {PPDs,Planets},
  month = mar,
  pages = 65,
  timestamp = {2014-07-25T17:17:29.000+0200},
  title = {{Protoplanetary Disks and Their Evolution}},
  url = {http://arxiv.org/abs/1103.0556},
  year = 2011
}