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<p><b style="font-weight:normal;"
id="docs-internal-guid-c411744a-c30c-f387-de7b-85ed6c2f6e35">Estimados,<br>
<br>
Les recordamos que hoy tendremos el siguiente seminario a las
13:00 hs. en </b><span style="font-weight:normal;">la Sala del
IALP. </span><b style="font-weight:normal;"
id="docs-internal-guid-c411744a-c30c-f387-de7b-85ed6c2f6e35"><br>
<br>
--<br>
Secretaría de Ciencia y Técnica<br>
FCAG</b></p>
<p><b style="font-weight:normal;"
id="docs-internal-guid-c411744a-c30c-f387-de7b-85ed6c2f6e35"><b>-----------------------------------------------------------------------------------------------------------------------------------------------------------------------</b></b></p>
<p><br>
<b style="font-weight:normal;"
id="docs-internal-guid-c411744a-c30c-f387-de7b-85ed6c2f6e35"><b
style="font-weight:normal;"
id="docs-internal-guid-696beaf9-cd25-5159-fecc-0b317a3c2b7a">
<p dir="ltr"
style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;"><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;"><b>Seminario: </b>M.Sc. Denny Hoyer </span></p>
<p dir="ltr"
style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;"><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">Estudiante de doctorado del "Institute for Astronomy and Astrophysics" Eberhard Karls University Tübingen.</span></p>
<br>
<p dir="ltr"
style="line-height:1.2;margin-top:0pt;margin-bottom:7pt;text-align:
justify;"><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:700;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">Título</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">: The giant-dwarf connection.</span></p>
<p dir="ltr"
style="line-height:1.2;margin-top:0pt;margin-bottom:7pt;text-align:
justify;"><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:700;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">Resumen</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">: The Asymptotic Giant Branch (AGB) phase is one of the most complex and yet not fully understood phase in stellar evolution. Spectral analyses of hydrogen-deficient AGB descendants yield constraints on nuclear</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">
</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">processes in that phase -- a pre-requisite to understand AGB stellar evolution.</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">
</span><span style="font-size:12pt;font-family:Verdana;color:#000000;background-color:transparent;font-weight:400;font-style:normal;font-variant:normal;text-decoration:none;vertical-align:baseline;white-space:pre-wrap;">The DO-type white dwarf RE 0503-289 was discovered in the ROSAT all-sky EUV survey two decades ago. Analyses of extreme and far-ultraviolet spectra of RE 0503-289 allowed to identify many metal lines up to the trans-iron elements. Thus, RE 0503-289 may be a rosetta stone to understand AGB nucleosynthesis and the post-AGB stellar evolution. To investigate its uniqueness, we selected three stars close to RE 0503-289 in the log T_eff-log g plane. These are the PG 1159-type star PG 1707+427 and the two DO-type white dwarfs PG 0109+111 and WD 0111+002. We present a NLTE spectral analysis and discuss their evolution.</span></p>
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