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Mariana Dominga Orellana

Researcher at National Scientific and Technical Research Council

Publications -  22
Citations -  604

Mariana Dominga Orellana is an academic researcher from National Scientific and Technical Research Council. The author has contributed to research in topics: Neutron star & Supernova. The author has an hindex of 8, co-authored 18 publications receiving 539 citations. Previous affiliations of Mariana Dominga Orellana include National University of Río Negro & IAR Systems.

Papers
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Journal ArticleDOI

Accretion vs. colliding wind models for the gamma-ray binary LS I +61 303: an assessment

Gustavo E. Romero, +3 more
- 01 Oct 2007 - 
TL;DR: In this paper, the authors apply a smoothed particle hydrodynamics (SPH) code in 3D dynamical simulations for both the pulsar-wind interaction and accretion-jet models.
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Structure of neutron stars in R-squared gravity

Mariana Dominga Orellana, +6 more
- 14 Feb 2013 - 
TL;DR: In this paper, a numerical integration of the structure equations that describe Neutron Stars (NSs) in strong gravity was performed, and it was shown that these profiles run in correlation with the second-order derivative of the analytic approximation to the Equation of State (EoS).
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Hadronic high-energy gamma-ray emission from the microquasar LS I +61 303

Gustavo E. Romero, +4 more
- 20 Oct 2005 - 
TL;DR: In this article, the gamma-ray emission originating from relativistic protons in the jet and cold protons from the wind was calculated for the microquasar LS I +61 303, which is formed by a neutron star that accretes matter from the dense and slow equatorial wind of the primary star.
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The unusual super-luminous supernovae sn 2011kl and asassn-15lh

Melina C. Bersten, +7 more
- 19 Jan 2016 - 
TL;DR: In this paper, the authors used the radiation hydrodynamics code to simulate magnetar-powered very luminous supernovae (SNe) and found that the light curve (LC) of SN 2011kl is consistent with a magnetar power source, but some amount of 56Ni is necessary to explain the low contrast between the LC peak and tail.
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High-energy neutrino emission from x-ray binaries

Hugo R. Christiansen, +2 more
- 29 Mar 2006 - 
TL;DR: In this article, high-energy neutrinos can be efficiently produced in X-ray binaries with relativistic jets and high-mass primary stars, where neutrino and correlated gamma-rays result from $pp$ interactions and the subsequent pion decays.