CV Lattes
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Universidade de São Paulo (USP). Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG) (Institutional affiliation from the last research proposal) Birthplace: Brazil
Physics Bachelor from Universidade de São Paulo (1995) and PhD in Astrophysics from Universidade de São Paulo (2001). Has experience on stellar astrophysics, with a focus on the following subjects: radiative transfer, numerical modeling, Be stars, and interferometry. (Source: Lattes Curriculum)
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The evolution of stars are shaped not only by their masses, but also by their metallicity. The chemical composition of a star will affect its formation, structure and evolution in complex ways, not fully understood yet. However, intriguing evidence propose that the emergence of fast-rotating stars is connected to low-metallicity environments. This project seeks to explore the correlation …
This 5-year project intends to apply high precision spectroscopy to study important problems in exoplanet science, stellar astrophysics and the Galaxy. Stars will be characterized using the line-by-line differential technique, in order to obtain precise chemical abundances with small errors of 0.01 - 0.02 in solar-metallicity stellar twins, or about 0.03 - 0.05 dex in metal-poor stars. Fu…
Astronomy in the 21st century continues to be a vibrant science; the more so as each decade passes. With the new generation of telescopes that is being currently planned, it will be possible to look for habitable Earth-like planets; to the inner regions of circumstellar disks, revealing the mechanisms that drive planetary and stellar formation; to resolve dense stellar populations in the …
This project aims at strengthening the collaborative ties between Prof. Alex Carciofi's group at the Universidade de São Paulo, and Prof. Michel Curé's group at Universidad de Valparaíso. Both groups share many interests in common and, most importantly, possess quite complementary competences. The applicants have already collaborated in the past, and with the present project this collabor…
Optical and infrared interferometry has allowed for great strides in many areas of astrophysics, in particular in stellar astrophysics, as it enables angularly resolved observations of nearby stars, providing unprecedented details about their photospheres and circumstellar environment. Pari passu with the observational advancements, there have been also quite significant advancements in n…
We propose an international collaborative research visit by Dr. Thomas Rivinius (European Southern Observatory, ESO/Chile) to the Universidade de São Paulo to strengthen and enhance the ongoing collaboration between him and Prof. Carciofi's research group (BeACoN) at the Departamento de Astronomia. During this visit we will finish writing a paper about the pre-periastron phase of the Be s…
(Only some records are available in English at this moment)
Recently, our research group at USP developed the first models of young stellar populations fully considering the Be phenomenon, in which a percentage of B-type stars in the population are rapid rotators and form circumstellar disks composed of matter expelled by the stars themselves. These new models, along with machine learning techniques, were applied to analyze data from the young clu…
Be stars are fast rotators and non-radial pulsators characterized by the presence of Keplerian circumstellar disks, consisting of material ejected by the star itself. Their variable behavior, controlled by mass loss events and complex viscous fluid dynamics in the disk, has been monitored through high-rate space photometry by satellites such as NASA's TESS. The resulting light curves show…
Be stars are main sequence B-type stars characterized by emission lines in their spectra. They exhibit high rotation rates and non-radial pulsations, resulting in the formation of an outwardly diffusing gaseous Keplerian disk. These disks cause the distinguishing observational features of Be stars, including emission lines, infrared excess, and linear polarization.Current models of Be sta…
(Only some records are available in English at this moment)
Recently, our research group at USP developed the first models of young stellar populations fully considering the Be phenomenon, in which a percentage of B-type stars in the population are rapid rotators and form circumstellar disks composed of matter expelled by the stars themselves. These new models, along with machine learning techniques, were applied to analyze data from the young clu…
Classical Be stars are fast rotating, non super-giant, B-type stars that have (or had at some moment) emission lines in their spectra. This emission feature is due to the reprocessing of ultraviolet light by a viscous decretion disk, ejected from the stellar equator by a still unknown mechanism that involves the near-critical rotation of the central star and maybe radial and non-radial pu…
Supergiant stars are massive, post-main sequence stars that lose large quantities of mass, forming a dense circumstellar outflow. Since they are cold, with effective temperatures between 3500 and 4500 K, large quantities of dust grains are formed in the ejected matter. The spectral energy distribution (SED) is usually the main source of information about the circumstellar dust in these ob…
(Only some records are available in English at this moment)
Be stars are fast rotating B type stars that, through the elusive Be phenomenon, eject mass into orbit, forming an equatorial viscous Keplerian disk. When a Be star is in a sufficiently close binary system, the presence of the companion can disrupt the Be disk. This includes the formation of two-armed structures, density waves, and, in its strongest form, disk truncation. While the compan…
My group in the Astronomy Department of IAG/USP specializes in Be stars. These stars, still in the main sequence, rotates very fast and, as a result, shed matter and angular momentum in their equatorial regions. This matter spreads out by means of viscous diffusion, thus forming a disk. Recently, we finished the first large-scale study of the dynamical evolution of a large sample of Be st…
HDUST is a radiative transfer code developed by prof. Carciofi (IAG/USP) in collaboration with prof. Jon Bjorkman (Univ. of Toledo, USA). This code was in the core of our research in the past decade or so, and its application in the field of Be star research allowed for important contributions in our understanding of the central object and its circumstellar disk. Recently, major advances …
(Only some records are available in English at this moment)
| 3 / 3 | Ongoing grants |
| 15 / 14 | Completed research grants |
| 4 / 4 | Ongoing scholarships in Brazil |
| 16 / 14 | Completed scholarships in Brazil |
| 5 / 4 | Completed scholarships abroad |
| 43 / 39 | All research grants and scholarships |
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