Asteroseismology of red giants & galactic archaeology

Red-giant stars are low- to intermediate-mass ($M \lesssim 10$~M$_{\odot}$) stars that have exhausted hydrogen in the core. These extended, cool and hence red stars are key targets for stellar evolution studies as well as galactic studies for several reasons: a) many stars go through a red-giant phase; b) red giants are intrinsically bright; c) large stellar internal structure changes as well as changes in surface chemical abundances take place over relatively short time; d) red-giant stars exhibit global intrinsic oscillations. Due to their large number and intrinsic brightness it is possible to observe many of these stars up to large distances. Furthermore, the global intrinsic oscillations provide a means to discern red-giant stars in the pre-helium core burning from the ones in the helium core burning phase and provide an estimate of stellar ages, a key ingredient for galactic studies. In this lecture I will first discuss some physical phenomena that play a role in red-giant stars and several phases of red-giant evolution. Then, I will provide some details about asteroseismology -- the study of the internal structure of stars through their intrinsic oscillations -- of red-giant stars. I will conclude by discussing galactic archaeology -- the study of the formation and evolution of the Milky Way by reconstructing its past from its current constituents -- and the role red-giant stars can play in that.Comment: Lecture presented at the IVth Azores International Advanced School in Space Sciences on "Asteroseismology and Exoplanets: Listening to the Stars and Searching for New Worlds" (arXiv:1709.00645), which took place in Horta, Azores Islands, Portugal in July 201

Solar Evolution Models with a Central Black Hole

Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10−6M⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions

Fauna epigeica em sistemas de produção de Nicotiana tabacum L.

O Rio Grande do Sul detém grande relevância na produção de tabaco. Adotam-se três sistemas de manejo: convencional, mínimo e plantio direto. Para analisar o impacto desses sistemas sobre a população da fauna do solo, efetuou-se uma amostragem da fauna epigeica. Foram avaliados preparo convencional (PC), cultivo mínimo (CM) e plantio direto (PD), além de área de reconversão da fumicultura para a vitivinicultura (RV) e de mata nativa (MN). Na amostragem, foram utilizadas dez armadilhas Provid em cada área. Os atributos avaliados foram: abundância de organismos, riqueza, índice de diversidade (H') e equitabilidade de Shannon (J). Collembola (Arthropoda: Hexapoda) foi identificada até o nível de família, devido à sua sensibilidade às modificações do ambiente. Efetuaram-se a análise multivariada de Agrupamento Hierárquico e a Análise de Componentes Principais, e os índices H' e J foram comparados pelo teste t, de Student. O PD apresentou maior número total de organismos, isolando-se das demais áreas pela análise de agrupamento hierárquico. Os valores de riqueza foram muito semelhantes entre as áreas, destacando-se a aproximação entre RV e MN. Os tratamentos PC, PD e RV não diferiram estatisticamente quanto ao H', apresentando valores de 1,58; 1,60; e 1,52, respectivamente. CM apresentou menor valor de H' (1,18) e MN, o valor intermediário (1,33). O comportamento estatístico de J foi muito semelhante ao encontrado em H'. Em relação à Classe Collembola, foram identificadas as famílias Entomobrydae, Sminthuridae, Poduridae e Hipogasturidae. PD apresentou exemplares das quatro famílias identificadas, enquanto nas demais áreas foram identificadas apenas Entomobrydae e Sminthuridae. Pela Análise de Componentes Principais (PCA), as diferenças entre as áreas explicaram 32 % da variabilidade encontrada; desse percentual, 59,3 % foram explicados pelos eixos 1 e 2. A presença ou ausência de revolvimento do solo e a rotação com culturas de cobertura foram os fatores que mais influenciaram as populações de fauna epigeica

TESS observations of cepheid stars: First light results

We present the first analysis of Cepheid stars observed by the TESS space mission in Sectors 1–5. Our sample consists of 25 pulsators: ten fundamental mode, three overtone and two double-mode classical Cepheids, plus three type II and seven anomalous Cepheids. The targets were chosen from fields with different stellar densities, both from the Galactic field and from the Magellanic System. Three targets have 2 minutes cadence light curves available by the TESS Science Processing Operations Center: for the rest, we prepared custom light curves from the full-frame images with our own differential photometric FITSH pipeline. Our main goal was to explore the potential and the limitations of TESS concerning the various subtypes of Cepheids. We detected many low-amplitude features: weak modulation, period jitter, and timing variations due to light-time effect. We also report signs of nonradial modes and the first discovery of such a mode in an anomalous Cepheid, the overtone star XZ Cet, which we then confirmed with ground-based multicolor photometric measurements. We prepared a custom photometric solution to minimize saturation effects in the bright fundamental-mode classical Cepheid, β Dor with the lightkurve software, and we revealed strong evidence of cycle-to-cycle variations in the star. In several cases, however, fluctuations in the pulsation could not be distinguished from instrumental effects, such as contamination from nearby sources, which also varies between sectors. Finally, we discuss how precise light-curve shapes will be crucial not only for classification purposes but also to determine physical properties of these stars. © 2021. The American Astronomical Society. All rights reserved