bibliography

2018

1. Impact splash chondrule formation during planetesimal recycling

   Tim Lichtenberg, Gregor J. Golabek, Cornelis P. Dullemond, and 3 more authors

   \icarus, Mar 2018

   Bib

   @article{2018Icar..302...27L,
     author = {{Lichtenberg}, Tim and {Golabek}, Gregor J. and {Dullemond}, Cornelis P. and {Sch{\"o}nb{\"a}chler}, Maria and {Gerya}, Taras V. and {Meyer}, Michael R.},
     title = {{Impact splash chondrule formation during planetesimal recycling}},
     journal = {\icarus},
     keywords = {Chondrule formation, Meteorites, Planetary formation, Planetesimals, Thermal histories, Astrophysics - Earth and Planetary Astrophysics, Physics - Geophysics},
     year = {2018},
     month = mar,
     volume = {302},
     pages = {27-43},
     doi = {10.1016/j.icarus.2017.11.004},
     archiveprefix = {arXiv},
     eprint = {1711.02103},
     primaryclass = {astro-ph.EP},
     adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..302...27L},
     adsnote = {Provided by the SAO/NASA Astrophysics Data System},
   }

2016

1. The effects of short-lived radionuclides and porosity on the early thermo-mechanical evolution of planetesimals

   Tim Lichtenberg, Gregor J. Golabek, Taras V. Gerya, and 1 more author

   Icarus, Mar 2016

   Abs Bib

   The thermal history and internal structure of chondritic planetesimals, assembled before the giant impact phase of chaotic growth, potentially yield important implications for the final composition and evolution of terrestrial planets. These parameters critically depend on the internal balance of heating versus cooling, which is mostly determined by the presence of short-lived radionuclides (SLRs), such as 26Al and 60Fe, as well as the heat conductivity of the material. The heating by SLRs depends on their initial abundances, the formation time of the planetesimal and its size. It has been argued that the cooling history is determined by the porosity of the granular material, which undergoes dramatic changes via compaction processes and tends to decrease with time. In this study we assess the influence of these parameters on the thermo-mechanical evolution of young planetesimals with both 2D and 3D simulations. Using the code family i2elvis/i3elvis we have run numerous 2D and 3D numerical finite-difference fluid dynamic models with varying planetesimal radius, formation time and initial porosity. Our results indicate that powdery materials lowered the threshold for melting and convection in planetesimals, depending on the amount of SLRs present. A subset of planetesimals retained a powdery surface layer which lowered the thermal conductivity and hindered cooling. The effect of initial porosity was small, however, compared to those of planetesimal size and formation time, which dominated the thermo-mechanical evolution and were the primary factors for the onset of melting and differentiation. We comment on the implications of this work concerning the structure and evolution of these planetesimals, as well as their behavior as possible building blocks of terrestrial planets.

   @article{LICHTENBERG2016350,
     title = {The effects of short-lived radionuclides and porosity on the early thermo-mechanical evolution of planetesimals},
     journal = {Icarus},
     volume = {274},
     pages = {350-365},
     year = {2016},
     issn = {0019-1035},
     doi = {https://doi.org/10.1016/j.icarus.2016.03.004},
     url = {https://www.sciencedirect.com/science/article/pii/S001910351600138X},
     author = {Lichtenberg, Tim and Golabek, Gregor J. and Gerya, Taras V. and Meyer, Michael R.},
     keywords = {Planetary formation, Terrestrial planets, Planetesimals, Interiors, Thermal histories}
   }

2. Isotopic enrichment of forming planetary systems from supernova pollution

   Tim Lichtenberg, Richard J. Parker, and Michael R. Meyer

   Monthly Notices of the Royal Astronomical Society, Aug 2016

   Abs Bib

   Heating by short-lived radioisotopes (SLRs) such as 26Al and 60Fe fundamentally shaped the thermal history and interior structure of Solar system planetesimals during the early stages of planetary formation. The subsequent thermo-mechanical evolution, such as internal differentiation or rapid volatile degassing, yields important implications for the final structure, composition and evolution of terrestrial planets. SLR-driven heating in the Solar system is sensitive to the absolute abundance and homogeneity of SLRs within the protoplanetary disc present during the condensation of the first solids. In order to explain the diverse compositions found for extrasolar planets, it is important to understand the distribution of SLRs in active planet formation regions (star clusters) during their first few Myr of evolution. By constraining the range of possible effects, we show how the imprint of SLRs can be extrapolated to exoplanetary systems and derive statistical predictions for the distribution of 26Al and 60Fe based on N-body simulations of typical to large clusters (103–104 stars) with a range of initial conditions. We quantify the pollution of protoplanetary discs by supernova ejecta and show that the likelihood of enrichment levels similar to or higher than the Solar system can vary considerably, depending on the cluster morphology. Furthermore, many enriched systems show an excess in radiogenic heating compared to Solar system levels, which implies that the formation and evolution of planetesimals could vary significantly depending on the birth environment of their host stars.

   @article{10.1093/mnras/stw1929,
     author = {Lichtenberg, Tim and Parker, Richard J. and Meyer, Michael R.},
     title = {{Isotopic enrichment of forming planetary systems from supernova pollution}},
     journal = {Monthly Notices of the Royal Astronomical Society},
     volume = {462},
     number = {4},
     pages = {3979-3992},
     year = {2016},
     month = aug,
     issn = {0035-8711},
     doi = {10.1093/mnras/stw1929},
     url = {https://doi.org/10.1093/mnras/stw1929},
     eprint = {https://academic.oup.com/mnras/article-pdf/462/4/3979/18756772/stw1929.pdf}
   }

1967

1. Vision

   

   Letters on wave mechanics

   Albert Einstein, Erwin Schrödinger, Max Planck, and 2 more authors

   Aug 1967

   Bib

   @book{przibram1967letters,
     title = {Letters on wave mechanics},
     author = {Einstein, Albert and Schrödinger, Erwin and Planck, Max and Lorentz, Hendrik Antoon and Przibram, Karl},
     year = {1967},
     publisher = {Vision},
   }

1956

1. 

   Investigations on the Theory of the Brownian Movement

   Albert Einstein

   Aug 1956

   Bib

   @book{einstein1956investigations,
     title = {Investigations on the Theory of the Brownian Movement},
     author = {Einstein, Albert},
     year = {1956},
     publisher = {Courier Corporation},
   }

1950

1. AJP

   The meaning of relativity

   Albert Einstein, and AH Taub

   American Journal of Physics, Aug 1950

   Bib

   @article{einstein1950meaning,
     title = {The meaning of relativity},
     author = {Einstein, Albert and Taub, AH},
     journal = {American Journal of Physics},
     volume = {18},
     number = {6},
     pages = {403--404},
     year = {1950},
     publisher = {American Association of Physics Teachers}
   }

1935

1. PhysRev

   Can Quantum-Mechanical Description of Physical Reality Be Considered Complete?

   A. Einstein^*†, B. Podolsky^*, and N. Rosen^*

   Phys. Rev., New Jersey. More Information can be found here , May 1935

   Abs HTML PDF Video

   

   In a complete theory there is an element corresponding to each element of reality. A sufficient condition for the reality of a physical quantity is the possibility of predicting it with certainty, without disturbing the system. In quantum mechanics in the case of two physical quantities described by non-commuting operators, the knowledge of one precludes the knowledge of the other. Then either (1) the description of reality given by the wave function in quantum mechanics is not complete or (2) these two quantities cannot have simultaneous reality. Consideration of the problem of making predictions concerning a system on the basis of measurements made on another system that had previously interacted with it leads to the result that if (1) is false then (2) is also false. One is thus led to conclude that the description of reality as given by a wave function is not complete.

1920

1. Relativity: the Special and General Theory

   Albert Einstein

   May 1920

   HTML

1905

1. Über die von der molekularkinetischen Theorie der Wärme geforderte Bewegung von in ruhenden Flüssigkeiten suspendierten Teilchen

   A. Einstein

   Annalen der physik, May 1905
2. Ann. Phys.

   Un the movement of small particles suspended in statiunary liquids required by the molecular-kinetic theory 0f heat

   A. Einstein

   Ann. Phys., May 1905
3. On the electrodynamics of moving bodies

   A. Einstein

   May 1905
4. Ann. Phys.

   Über einen die Erzeugung und Verwandlung des Lichtes betreffenden heuristischen Gesichtspunkt

   Albert Einstein

   Ann. Phys., May 1905

   Nobel Prize Abs Bib

   Albert Einstein receveid the Nobel Prize in Physics 1921 for his services to Theoretical Physics, and especially for his discovery of the law of the photoelectric effect

   This is the abstract text.

   @article{einstein1905photoelectriceffect,
     title = {{{\"U}ber einen die Erzeugung und Verwandlung des Lichtes betreffenden heuristischen Gesichtspunkt}},
     author = {Einstein, Albert},
     journal = {Ann. Phys.},
     volume = {322},
     number = {6},
     pages = {132--148},
     year = {1905},
     doi = {10.1002/andp.19053220607},
   }