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Os elementos químicos : do Big Bang aos planetas rochosos
The chemical elements :
from the Big Bang to terrestrial planets
Jorge Meléndez Departamento de Astronomia do IAG/USP
Be C
O S
F
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First elements in the universe:
H, He, Li
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Evolution of our universe First few minutes: H, He, Li
Big Bang
tim
e
13,7 billion years
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The abundances of
the light elements
(H, He, Li) formed a
few minutes after
the Big Bang
depend only on η10 (baryon-to-photon ratio)
credits: NASA η10
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Evolution of our universe Cosmic Background Radiation
Big Bang
tim
e
13,7 billion years
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Cosmic Background Radiation
credits: NASA
T = 2.725 ± 0.001 K
small fluctuations in the
cosmic radiation η10
WMAP
satellite
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The abundances of
the light elements
(H, He, Li) formed a
few minutes after
the Big Bang
depend only on η10 (baryon-to-photon ratio)
credits: NASA η10
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8
credits: http://map.gsfc.nasa.gov
Cosmic Microwave Background
η10 = 6.226 0.170
A(Li) = 2.72 dex Li/H = 5.2 10-10
Predicted primordial lithium abundance:
WMAP
(Cyburt et al. 2008, see also Steigman 2009; Coc & Vangioni 2010)
Bh2 = 0.02273±0.00062
(Dunkley et al. 2009)
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9
To test Big Bang Nucleosynthesis we need
to look back in time: metal-poor stars
credits: N. Christlieb
Rela
tive
flu
x
Wavelength
Sun: [Fe/H] = 0
solar metallicity
CD-38 245: [Fe/H] = - 4 (10-4 solar)
HE 0107-5240: [Fe/H] = - 5.3
Population III: [Fe/H] = - ∞
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Spite & Spite (1982)
Primordial Li in metal-poor stars !
Wavelength
Re
lati
ve F
lux
Asplund et al. (2006)
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11
Stars (Li = 2.0 – 2.25)
Aoki et al. (2009)
2.7
LITHIUM in STARS:
Triangles: Asplund et al 2006
Squares: Bonifacio et al. 2007
Filled Circles: Aoki et al. 2009
WMAP+ BBN
Cosmological lithium problem
WMAP+ BBN (Li = 2.72)
0.7 dex (factor of 5) discrepancy at the lowest metallicities between BBN+WMAP and stars
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12
The cosmological Li problem: Li in stars is much lower (x 5) than
the primordial Li predicted by BBN
Teff scale
Errors in nuclear reaction rates
New physics / cosmology ?
Li depletion in stars ?
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Ultra high precision analysis
of lithium in metal-poor stars
Hawaii, after observing run ...
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Ultra high precision analysis of
lithium in metal-poor stars using
Keck and VLT data Stellar spectrum observed with Keck (exposure time of 5 hours)
Asplund & Melendez (2008)
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15
Next steps in solving the Li problem
@ IAG/USP Finish data reduction
Accurate + precise stellar parameters
Determination of Li and Be abundances
Study of Li and Be depletion
Li isotopes
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16
Solving the cosmological Li problem Team : Jorge Melendez (IAG)
Martin Asplund (Australia)
Luca Casagrande (Australia)
Ivan Ramirez (Carnegie, USA)
Help
Welcome !
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Periodic Table of the Astronomers ..
From H and He to “metals”
METALS
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Chemical evolution of the elements
From H and He to “metals”
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The first stars and the formation of
metals (elements
heavier than H & He)
Primordial
clouds
H, He Supernova: metal-rich ejecta
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Stellar Evolution Type II
supernova
Type Ia supernova (artist’s concept)
Planetary nebula
O
Fe
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Galactic chemical evolution
H, He
Metal-rich
ejecta
stars
Inte
rste
llar
med
ium
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After 12 billion years of chemical evolution in
our Galaxy, stars have produced only 2% of
“metals”, the rest (98%) being H & He
Our solar system
The Milky Way
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Galactic archaeology
OLD POPULATIONS
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Galactic archaeology: disk(s) [a
-ele
ments
/Fe] Thick disk (old disk)
Thin disk (young disk)
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Galactic archaeology: bulge [a
-ele
ments
/Fe]
Thick disk ~ Bulge
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Galactic archaeology: halo(s)
Bulge
Nissen &
Schuster 2010
“true” halo
stars?
from dSph
galaxies ?
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High precision chemical
abundances in metal-poor stars
@ IAG / USP High resolution (R = 100, 000) high S/N spectra (300-1000)
available to perform the highest precision study to date
HELP
WELCOME !
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Looking for planetary systems like our own
Sunset in Paracas, Peru (c) www.flickr.com/photos/rodrigocampos/
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More than 500 planetary systems found until now
But ... most of
them DO NOT
resemble our own
solar system
C. Carreau / ESA
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Most planetary systems found so far have inner giant planets, unlike the inner rocky planets of
our solar system
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How to find a planetary system similar to our own?
Credits: Nasa
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1. Search for stars similar to our Sun Sol = 1 pixel
Betelgeuse Antares
Aldebaran
Rigel
Arcturus Pollux
Sirius Sol
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2. In the same evolutionary stage as our Sun
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3. Chemical composition ~ solar?
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But there are myriad stars in the sky … how can we find solar twins?
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Diagrama H-R
SOL
Mv = 4.82
B-V ~ 0.65
Indice de cor
Ma
gn
itu
de
ab
so
luta
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Procura por gêmeas solares usando o catálogo Hipparcos (+ Tycho)
•Cores BT-VT
•Magnitude absoluta VT
• Outras cores (optico e infravermelho), indicadores de idade
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• Nos primeiros 25 anos de pesquisa não foi encontrada nenhuma gêmea solar (Cayrel de Strobel et al. 1996)
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First solar twin discovered only in 1997: 18 Sco
18 Sco
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Searching for solar twins
• Programa observacional desde 2005
- Keck (Havaí, USA)
- McDonald (Texas, USA)
- Magellan (Chile)
- VLT/UVES (Chile)
- La Silla / HARPS (Chile)
Colaboração: Australia, França, Portugal, U.S.A., Brasil, Chile, México, Inglaterra, Alemanha
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Second solar twin identified in 2006: HD 98618
- Undergrad summer research project of Katie Dodds-Eden
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HD 98618: Destaque na imprensa
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Mas 18 Sco e HD 98618 não são gêmeas solares perfeitas …
• Abundancias de lítio são muito altas, um fator de 3 maior que no Sol !
Estrela - Sol
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Continuing the search for perfect solar twins: McDonald
• 2.7-m tel. + 2dcoudé
• Observações em Abril, Out, Nov 2007
• P.I.: Iván Ramírez
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McDonald solar twin survey Novas gêmeas solares HIP 56948 &
HIP 73815 tem baixo Li (~1.0)!
Muito parecido ao Sol !
(Melendez et al. 2006;Melendez & Ramirez
(07
HIP 56948 é a
melhor gêmea
solar, quase
identica ao Sol,
inclusive no lítio.
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HIP 56948: destaque na imprensa
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HIP 56948: destaque na imprensa
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Is the Sun a normal solar-type star? Are there any anomalies in the Sun’s chemical composition?
© ESA/NASA/SOHO
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Por quase um seculo e meio o Sol foi considerado ”normal” na sua
composição química
• Secchi (1868): Sol é tipico de estrelas de tipo solar
• Payne (1925): composição solar é universal
• Bent Gustafsson (1998, 2008): não sabemos devido às grandes incertezas (0.05-0.10 dex)
• Carlos Allende Prieto (IAU Symp 265 [Aug09] revisão sobre o disco fino): devemos melhorar nossas abundancias: <0.05 dex (accuracy)
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High precision chemical abundance study of solar twins:
Magellan (Clay 6.5m)
Jorge Meléndez (CAUP/Portugal), Martin Asplund (Max Planck),
Bengt Gustafsson (Uppsala), David Yong (Stromlo)
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Observações espectroscópicas -Magellan 6.5m Clay Telescope
& Mike spectrometer
- R = l/Dl = 65,000
- S/N = 450 per pixel
- coverage 340 – 1000 nm
- Solar spectrum:asteroid Vesta
- 3 nights of observations.
BLUE frame RED frame
Observações da gêmea solar 18 Sco
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Small part
(597-603nm)
of solar twin &
Sun’sspectra
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Our Sun is
abnormal !
Abundancias no
Sol - <gêmeas>
vs. número
atómico Z
Sol típico:
Δ = 0
Sol anormal:
Δ ≠0
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Are the anomalies in the Sun’s composition related to the formation of
our planetary system ?
The Sun & the Andes from the windows of Machu Picchu http://www.flickr.com/photos/oscarpacussich
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~ 0.08 dex ~ 20% Correlação é
altamente
significativa
probabilidade ~10-9
de acontecer por
acaso
Anomalias no
Sol são
fortemente
correlacionadas
com a
temperatura de
condensação
(Tcond) dos
elementos!
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Somente os elementos refractarios (e.g. Fe, Al, Sc) podem ter se condensado no
sistema solar interno, forming dust, planetesimals and finally rocky planets
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As camadas externas do Sol acretaram material deficiente em refractarios
Iron gradient in the inner solar system
O Sol é deficiente
em refratarios
porque esses
elementos foram
usados para formar
os planetas
terrestres!
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Relação com formação de
planetas terrestres:
meteoritos
O comportamento
do Sol é uma
imagem espelho
do seguido por
meteoritos!
Alexander
et al. (2001)
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How much dust-cleansed gas is required to affect
the Sun in this way?
Assume gas accretion until
solar convection zone reached
~ present size (~0.02 Msun):
Refractories depleted in the
Sun: ~2*1028 g ≈ 4 M
Refractories locked-up in
terrestrial planets:
~8*1027 g ≈ 1.3 M
A quantidade de material que falta no Sol
é da mesma ordem que a requerida para
formar os planetas terrestres + asteroides
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O manto terrestre
também mostra
abundancias
compativeis com
o nosso cenario volatileelementsinEarth’s
mantle are depleted !
DepletiontrendofvolatilesinEarth’s
mantle probably reflects primary
nebular depletion in the Earth making
material (Witt-Eickschen et al. 2007).
Earth-making material was poor in
volatiles, and the Sun rich in
refractories !
Witt-Eickschen et al. (2007)
Lithophile:
silicate loving
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O Sol é unico ?
Não, o Sol é peculiar mas não é unico: ~ 10-20% de estrelas de tipo solar tem uma composição química similar ao Sol, e tal vez possam possuir planetas como a nossa Terra (e tal vez vida !)
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Destaques na imprensa sobre a composição peculiar do Sol
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Destaques na imprensa sobre a composição peculiar do Sol
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Solar twins @ IAG/USP
Sol – g
êm
eas s
ola
res
Temperatura de
condensação
Extremely high precision abundance analysis using Keck and VLT data
to study signatures
of planet formation
Meléndez,
Asplund,
Gustafsson,
Yong 2009,
ApJ letters
Tala Monroe (new postdoc @ IAG/USP)
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Solar twins @ IAG/USP Biogenic elements :
C, O, N, P, S
(Basic building blocks of life)
using VLT CRIRES data
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O estudo se viabilizou graças ao acesso recém-obtido pelo Brasil
às instalações do ESO (Observatório Europeu do Sul). O
governo assinou no fim do ano passado o acordo que torna o país o mais novo membro do
consórcio. Embora o acerto ainda careça de aprovação do
Congresso para entrar em vigor, o ESO já trata o Brasil como
parceiro, concedendo o direito de solicitar tempo de observação nos telescópios da organização.
Foi por conta disso que a equipe de Jorge Meléndez, peruano que
trabalha no IAG (Instituto de Astronomia, Geofísica e Ciências Atmosféricas) da USP, conseguiu
aprovação num projeto que pode finalmente revelar alguns dos segredos mais bem guardados
sobre os exoplanetas.
Procura de planetas ao redor de gêmeas solares: 88 noites no HARPS/ESO
Help most welcome
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CONCLUSIONS Very exciting research @ IAG/USP related to the chemical composition of stars:
• Big Bang nucleosynthesis
• Galaxy formation and evolution
• Stellar evolution
• Planet formation
• Uniqueness of our Sun and our solar system
• Others: M dwarfs, isotopic ratios, stellar clusters, molecular spectroscopy, giant stars with planets, stellar parameters, interstellar extinction, archaeoastronomy...