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Mayra has been working at the Instituto de Astrofísica de Andalucía – CSIC since 2002. She is originally from Veracruz, Mexico, and studied physics at Veracruz University, finishing her PhD studies at the National Autonomous University of Mexico (UNAM), Mexico. After which she achieved her Postdoc at the Harvard & Smithsonian Center for Astrophysics.
Mayra has been working at the Instituto de Astrofísica de Andalucía – CSIC since 2002. She is originally from Veracruz, Mexico, and studied physics at Veracruz University, finishing her PhD studies at the National Autonomous University of Mexico (UNAM), Mexico. After which she achieved her Postdoc at the Harvard & Smithsonian Center for Astrophysics.
Mayra was a pioneer in the modelization of the earliest phases of massive stars, which are called hot molecular cores (Osorio et al 1999 ApJ. 525, 808, Osorio et al. 2009, ApJ. 694, 29). Currently Mayra’s research is focused on stellar and planetary formation. She likes planet formation in extreme conditions, such as those found around massive stars, in multiple systems or in very tiny disks, as well as the survival of planets around evolved stars (post AGB type). For these studies, she models emblematic cases in great detail, using radiative transfer codes in order to reproduce the emission coming from their circumstellar envelopes and accretion disks. She also observes these objects at a very high angular resolution using data obtained primarily from the large interferometers.
Mayra is also interested in studying a large number of young stars like those to be found in Orion, where protostars of different luminosities are born in diverse physical conditions, and in an isolated or cluster form. She belongs to the Herschel Orion Protostar Survey (HOPS) team, where more than 300 young protostars have been identified, and which have been observed with the infrared spectrum of Spitzer, Herschel, Sofia and in radio wavelengths with ApeX, ALMA and VLA.
The Herschel Orion Protostar Survey (HOPS)
Modeling a unique accretion disk around a high-mass protostar
Non‐thermal radio emission from the jet associated with an intermediate-mass protostar
HL Tau’s neighbouring binary, XZ Tau, was born from dwarf disks
HL Tau’s neighboring star is born from a dwarf disk
Mayra was a pioneer in the modelization of the earliest phases of massive stars, which are called hot molecular cores (Osorio et al 1999 ApJ. 525, 808, Osorio et al. 2009, ApJ. 694, 29). Currently Mayra’s research is focused on stellar and planetary formation. She likes planet formation in extreme conditions, such as those found around massive stars, in multiple systems or in very tiny disks, as well as the survival of planets around evolved stars (post AGB type). For these studies, she models emblematic cases in great detail, using radiative transfer codes in order to reproduce the emission coming from their circumstellar envelopes and accretion disks. She also observes these objects at a very high angular resolution using data obtained primarily from the large interferometers.
Mayra is also interested in studying a large number of young stars like those to be found in Orion, where protostars of different luminosities are born in diverse physical conditions, and in an isolated or cluster form. She belongs to the Herschel Orion Protostar Survey (HOPS) team, where more than 300 young protostars have been identified, and which have been observed with the infrared spectrum of Spitzer, Herschel, Sofia and in radio wavelengths with ApeX, ALMA and VLA.
Envolturas de polvo en torno a estrellas masivas
Disk models in low and high-mass protostar
Discos de polvo en torno a estrellas jóvenes (masa baja e intermedia)
The Herschel Orion Protostar Survey (HOPS)
Modeling a unique accretion disk around a high-mass protostar
Non‐thermal radio emission from the jet associated with an intermediate-mass protostar
HL Tau’s neighbouring binary, XZ Tau, was born from dwarf disks
HL Tau’s neighboring star is born from a dwarf disk
