CNO abundances in the Sun and Solar Twins

Size: px
Start display at page:

Download "CNO abundances in the Sun and Solar Twins"

Transcription

1 CNO abundances in the Sun and Solar Twins Jorge Meléndez Departamento de Astronomia, IAG, Universidade de São Paulo Sunset in Paracas, Peru (c)

2 Why are C, N, O (and Ne) important? After H (X) and He (Y), they are the most abundant elements, so they have a crucial impact on the mass fraction of metals Z (elements heavier than H, He) H He O C Ne F Mg N Al Na Si Fe Asplund et al X + Y + Z = 1. B Li Be

3 The metallicity Z is important for the morphology of evolutionary tracks and isochrones VandenBerg et al VandenBerg et al. 2007

4 Solar models vs. helioseismology E = log(n E /N H ) + 12 O, C, N (dex) + meteoritic 8.86, 7.92, , 7.83, , 7.83, photospheric 8.66, 7.78, 8.39 GS98: Grevesse & Sauval 1998 AGS05 : Asplund et al AGSS09 : Asplund et al Serenelli et al. 2009

5 Solar Oxygen Abundance What is going on with the solar O abundance? Anders & Grevesse ± ±0.07 Caffau et al ±0.05 Asplund et al ±0.05 Asplund et al. 2009

6 Solar carbon abundance What about carbon? Anders & Grevesse 1989 Grevesse & Sauval 1998 Caffau et al Asplund et al Asplund et al Year

7 Solar nitrogen abundance What about nitrogen? Anders & Grevesse 1989 Grevesse & Sauval 1998 Caffau et al Asplund et al Asplund et al Year

8 Why are the Asplund, Grevesse & Sauval (2005) solar C, N, O abundances very low? 1) Improvements in the measurements on the solar spectra (blends with other species). Forbidden [OI] line at 6300 A Allende Prieto, Lambert, Asplund (2001) A(O)=8.69±0.05 3D

9 ( dex BLEND with NiI (-0.13 TRANSITION PROBABILITIES FOR THE [OI] 6300 A line : Old log gf = New log gf = Difference in abundance: dex 3D-1D: Why are the Asplund et al. (2005) solar C, N, O abundances very low? 2) Improvements in the atomic data (transition probabilities) 3) Improvements in the model atmospheres (3D hydro) After blends + new gf-value + 3D : A(O) = 8,69 dex But ignoring 3D+blend+better data, A(O)=8,92 dex -Allende Prieto, Lambert & Asplund 2001, ApJ, 556, L63 -Asplund et al. 2004, A&A, 417, 751

10 Why Asplund et al. (2005) C, N, O are low? 4) Departures from local thermodynamic equilibrium accounted for (mostly). A(O)= 8.88 [LTE] Permitted lines: 777 nm OI triplet A(O)=8.66, 8.72 [NLTE] S H =0, 1 NLTE corrections ~ -0.2 dex 8.88 [LTE] Center / limb variation of OI 8.66 [NLTE] Allende Prieto, Asplund & Fabiani ( 2004 ) Bendicho 8.72 [NLTE] ( 1968 ) NLTE effects on OI 777nm already suggested by Altrock

11 Revision of Asplund et al. (2005): new solar CNO with improved 3D models (Asplund et al. 2009) The temperature gradient of the Asplund et al. (2005) 3D solar model atmosphere seem to be too step when compared to observations of the center-to-limb variation (Ayres et al. 2006; Koesterke et al. 2008). Disk center The new 3D model by Asplund et al. (2009) has much improved radiative transfer and updated opacities. The new model is in excellent agreement with the center-to-limb variation observed in the Sun. Asplund et al. (2009) Limb

12 Latest set of C, N, O abundances from Asplund, Grevesse, Sauval & Scott (2009) C = 8.43 N = 7.83 O = 8.69 Excellent agreement between atomic and molecular lines

13 What about other 3D models? Excellent agreement between Stagger (Asplund et al.) and CO 5 BOLD (Caffau et al.) codes Caffau et al Asplund et al. 2009

14 Independent analyses by the Caffau et al. group (Caffau, Ludwig, Steffen, Freytag et al.) using 3D CO 5 BOLD models Element Caffau et al. (2008, 2009, 2010) Asplund et al. (2009) Carbon 8.50+/ /-0.05 Nitrogen 7.86+/ /-0.05 Oxygen 8.76+/ /-0.05 Good agreement on N, but not so good for O and C

15 Caffau et al. (2009) nitrogen abundance Used equivalent widths from the literature (Grevesse et al.) + CO 5 BOLD 3D model + NLTE Only atomic lines were analyzed by Caffau et al. (Asplund et al. analyzed atomic and molecular lines) Caffau et al. (2009) Asplund et al. (2009) 7.86+/ /-0.05 Agreement!

16 Caffau et al. (2010) carbon abundance Used their own measurements of equivalent widths + CO 5 BOLD 3D model + NLTE Only atomic lines were analyzed by Caffau et al. (Asplund et al. used atomic and molecular lines) Caffau et al. (2010) Asplund et al. (2009) 8.5+/ /-0.05 disagreement! Main reason for discrepancy is probably the different set of equivalent width measurements used by both groups.

17 Caffau et al. (2008) oxygen abundance Used their own measurements of equivalent widths + CO 5 BOLD 3D model + NLTE Only atomic lines were analyzed by Caffau et al. (Asplund et al. used atomic and molecular lines) Caffau et al. (2008) Asplund et al. (2009) 8.76+/ /-0.05 Caffau et al. like disagreement! H.-G. Ludwig, 2012 Main reason for discrepancy is the different set of equivalent width measurements used by both groups.

18 Good agreement for N, but who is more likely to be right (if any) regarding C and O? Element Caffau et al. (2008, 2009, 2010) Asplund et al. (2009) Carbon 8.5+/ /-0.05 Nitrogen 7.86+/ /-0.05 Oxygen 8.76+/ /-0.05 We urgently need a new independent study of the photospheric CNO solar abundances

19 An independent study of C, N, O in the Sun (Meléndez, in preparation, 2012?) - Selection of only best lines (not always possible) - Detailed evaluation of blends (mainly CN) - Careful measurements - Most recent atomic data - Using only telluric-corrected solar spectra (red, IR) - New optical-near IR flux atlas by Wallace et al Complemented in the IR by disk center atlas by Wallace et al. (1993)

20 Relative flux An independent study of C, N, O in the Sun (Meléndez, in prep., 2012?) Good knowledge of molecular line formation is needed to take into account blends. CN is ubiquitous in the solar spectrum Wavelength (A) Meléndez, in preparation

21 Relative flux Relative flux CN is ubiquitous in the solar spectrum 1.00 (Meléndez, in prep., 2012?) Wavelength (A) CN line list from Meléndez & Barbuy (1999)

22 CN blends for O I triplet (Meléndez, in preparation) CN blends must be taken into account, otherwise the equivalent widths may be overestimated or underestimated CN CN CN CN Other blend CN CN

23 Comparison of equivalent widths for O I triplet Line (A) Asplund E.W. (A) Asplund et al. A(O) Caffau E.W.(A) Caffau A(O) Melendez E.W. Melendez A(O) ? ± ? ± ? ± average 8.69 dex? 8.75 dex 8.74 dex (Meléndez, in preparation) Asplund et al. E.W. may be underestimated by 3,5% Caffau et al. equivalent widths may be overestimated by 8,2% Caution: final result depends on adopted NLTE corrections (uncertain at least ~ 0,03 dex)

24 What about the forbidden [OI] lines? 6300 A line: badly blended with Ni I. Uncertain correction A line: blended with CN. Very preliminary result, A(O) ~ A line: blended with C 2. Very preliminary result, A(O) ~ 8.7

25 5577 A [OI] line! Blend by C 2 easily constrained by red side of the feature. O and C abundances determined at the same time! revised Melendez & Asplund (2008). To be

26 VERY PRELIMINARY RECOMMENDED OXYGEN ABUNDANCE (molecular OH lines will be included later) Oxygen triplet at 777nm : 8,74 dex Forbidden [OI] lines 6363, 5577 A : 8,7 dex Suggested solar O abundance : Meléndez (in prep.) : 8,72 dex Caffau et al. 2008: 8,76 dex Asplund et al : 8,69 dex

27 What about carbon? Also, we must be careful about blends with CN lines Example : C I lines at 7111,4 and 7113,2 A CN CN CN CN CN CN CN CN CN CN C I C I

28 VERY PRELIMINARY RECOMMENDED CARBON ABUNDANCE (based on permitted lines and one [C I] line. Molecular lines to be included later) Suggested solar C abundance : Meléndez (in prep.) : 8,40 dex Caffau et al. 2008: 8,50 dex Asplund et al : 8,43 dex

29 VERY PRELIMINARY RECOMMENDED NITROGEN ABUNDANCE (based on permitted lines. Molecular lines to be included later) Suggested solar N abundance : Meléndez (in prep.) : 7,82 dex Caffau et al. 2008: 7,86 dex Asplund et al : 7,83 dex

30 Summary on C, N, O solar abundances Element Caffau et al Asplund et al. (2009) Meléndez (2012?) GS98 Carbon 8.50+/ / ,40 8,52 Nitrogen 7.86+/ / ,82 7,92 Oxygen 8.76+/ / ,72 8,83 high thetoreturntounlikelyseemsitdatacurrenttheonbased Grevesse & Sauval (1998) C, N, O abundances

31 Sunset in Paracas, Peru (c) Is it correct to assume the solar abundance pattern for other stars? Solar twins can tell us how typical is the Sun

32 Magellan ultra high precision study of Observations of the solar twin 18 Sco solar twins -Magellan 6.5m Clay Telescope & Mike spectrometer - R = 65,000 - S/N = 450 per pixel - coverage nm - Solar spectrum: Vesta - 3 nights of observations BLUE frame RED frame -Meléndez et al

33 Example of Magellan spectra (total spectral coverage 3400 A -1um) Small part ( nm) of solar twin & Sun s spectra -Meléndez et al

34 Δabundance: Sun - <twins> vs. atomic number Z Sun typical : Δ = 0 Sun weird : Δ 0 Our solar system is not host by a typical Sun Melendez et al

35 Sun s anomalies are strongly correlated to condensation temperature (T cond ) of the elements! Correlation is highly significant probability ~10-9 to happen by chance ~ 0.08 dex ~ 20% It s most likely to win the lottery Condensation temperature Melendez et al

36 Condensation Condensation in the solar nebula Mercury Venus 36

37 The late accreted gas in the convection zone was deficient in refractories The late-accreted Sun stheingas convection zone was depleted in refractories which were used to form dust, planetesimals & terrestrial planets Iron gradient in the inner solar system 37

38 Either 1) the Sun is normal in the volatile C, N, O AND depleted in the refractory elements (e.g. Fe, Al, Ni) or 2) the Sun is normal in the refractories but enhanced in the volatiles (CNO) Option (1) is most likely correct ~ 0.08 dex ~ 20% Condensation temperature Melendez et al. 2009

39 Results on solar anomalies confirmed by others. Our Sun is indeed chemically peculiar, perhaps due to the formation of terrestrial planets The Sun may be more metal-rich in its interior! Meléndez et al

40 What about the effect of giant planet formation? 16 Cyg pair of solar analogs 16 Cyg A : no planets 16 Cyg B : giant planet 40

41 16 Cyg B (planet-host) is 0,04 dex more metalpoor in all elements (photospheric abundances)! Was the missing material used to form the giant planet around the solar analog 16 Cyg B? Is 16 Cyg B more metal-rich in its interior? 41

42 Conclusions Solar C, N, O abundances seem intermediate between the values of Asplund et al (2009) and Caffau et al. (2008, 2009, 2010), although somewhat closer to Asplund et al. Sun may be more metal-rich in its interior, with refractory elements about 0,08 dex more abundant than in its photosphere (terrestrial planet effect) Sun may be more metal-rich in its interior for ALL ELEMENTS by another 0,04 dex (giant planet effect) In summary, Sun may be richer in its interior by 0,12 dex for refractory elements and 0,04 dex for volatile CNO elements. It is urgent to estimate the Sun s abundances in its interior. 42

From the first stars to planets

From the first stars to planets High precision stellar spectroscopy: From the first stars to planets Jorge Meléndez Departamento de Astronomia, IAG, Universidade de São Paulo My group: SAMPA Stellar Atmospheres, Planets & Abundances

More information

Galac%c Unprecedented Precision (0.01 dex)

Galac%c Unprecedented Precision (0.01 dex) Li Be B Si O Fe Dy Ce Ru Y Pb C a Ti L V b Y Eu Al N Pr d Sr Mo Ba P Ca K Cr S N Sm Gd U Ag Pd Mg Ni Galac%c Archaeology @ Unprecedented Precision (0.01 dex) @DrJorgeMelendez Dep. Astronomia, Univ. São

More information

Solar Neutrinos and The Sun NEUTEL 11 Venice 15/03/11

Solar Neutrinos and The Sun NEUTEL 11 Venice 15/03/11 Solar Neutrinos and The Sun NEUTEL 11 Venice 15/03/11 A. Serenelli Outline Update on Solar models: abundances and nuclear reaction rates Solar neutrino fluxes from neutrino data: can neutrinos disentangle

More information

The Standard Solar Model. PHYSUN L'Aquila

The Standard Solar Model. PHYSUN L'Aquila The Standard Solar Model Aldo Serenelli Max Planck Institute for Astrophysics PHYSUN L'Aquila 16-17 October, 2008 Outline Overview of Standard Solar Model - BPS08 Two solar compositions SSM, solar compositions

More information

The chemical composition of the Sun

The chemical composition of the Sun Astrophys Space Sci (2010) 328: 179 183 DOI 10.1007/s10509-010-0288-z ORIGINAL ARTICLE The chemical composition of the Sun N. Grevesse M. Asplund A.J. Sauval P. Scott Received: 5 October 2009 / Accepted:

More information

The impact of solar surface dynamo magnetic fields on the chemical abundance determination

The impact of solar surface dynamo magnetic fields on the chemical abundance determination The impact of solar surface dynamo magnetic fields on the chemical abundance determination N. Shchukina 1, A. Sukhorukov 1, J. Trujillo Bueno 2 1 Main Astronomical Observatory, National Academy of Sciences,

More information

Oxygen in the Early Galaxy: OH Lines as Tracers of Oxygen Abundance in Extremely Metal-Poor Giant Stars

Oxygen in the Early Galaxy: OH Lines as Tracers of Oxygen Abundance in Extremely Metal-Poor Giant Stars Oxygen in the Early Galaxy: OH Lines as Tracers of Oxygen Abundance in Extremely Metal-Poor Giant Stars A. Kučinskas 1, V. Dobrovolskas 1, P. Bonifacio 2, E. Caffau 2, H.-G. Ludwig 3, M. Steffen 4, M.

More information

The Connection between Planets and the Stellar Chemical Composition

The Connection between Planets and the Stellar Chemical Composition The Connection between Planets and the Stellar Chemical Composition Lorenzo Spina Universidade de São Paulo, IAG, Departamento de Astronomia - Brazil Credits: NASA Jupiter Saturn Neptune Uranus Venus Earth

More information

Oxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto!

Oxygen in red giants from near-infrared OH lines: 3D effects and first results from. Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Oxygen in red giants from near-infrared OH lines: 3D effects and first results from Puerto de la Cruz, May 14, 2012! Carlos Allende Prieto! Overview! 1. APOGEE: status and prospects! 2. A first look at

More information

Differential abundances in the HAT-P-4 binary system

Differential abundances in the HAT-P-4 binary system Differential abundances in the HAT-P-4 binary system Carlos Saffe 1,4, Emiliano Jofré 2,4, Eder Martioli 3 Matías Flores 1,4, Romina Petrucci 2,4 & Marcelo Jaque 1,4 (1) Instituto de Ciencias Astronómicas,

More information

The new solar abundances - Part II: the crisis and possible solutions

The new solar abundances - Part II: the crisis and possible solutions Comm. in Asteroseismology Vol. 147, 2006 The new solar abundances - Part II: the crisis and possible solutions J.Montalbán 1, A. Miglio 1, S. Théado 1, A. Noels 1, N. Grevesse 1,2 1 Institut d Astrophysique

More information

Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg"

Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg" Spectroscopy of (cool) giants and supergiants! Maria Bergemann MPIA Heidelberg" Outline! Motivation why do spectroscopy of giant

More information

Neutrinos and Solar Metalicity

Neutrinos and Solar Metalicity Neutrinos and Solar Metalicity The solar abundance problem and CN neutrinos Measurement opportunities Wick Haxton INT 8 June 2015 The Standard Solar Model Origin of solar neutrino physics: desire to test

More information

Lecture 31. Planetary Accretion the raw materials and the final compositions

Lecture 31. Planetary Accretion the raw materials and the final compositions Lecture 31 Planetary Accretion the raw materials and the final compositions Reading this week: White Ch 11 (sections 11.1-11.4) Today 1. Boundary conditions for Planetary Accretion Growth and Differentiation

More information

Star-planet connection:

Star-planet connection: : The role of stellar metallicity Centro de Astrofísica da Universidade do Porto Instituto de Astrofísica e Ciências do Espaço 18 September 2014 Porto, Portugal 1 Planet formation and metallicity Giant

More information

arxiv: v1 [astro-ph.sr] 23 Jan 2015

arxiv: v1 [astro-ph.sr] 23 Jan 2015 Astronomy& Astrophysics manuscript no. oxygen c ESO 2015 January 26, 2015 Oxygen abundances in G- and F-type stars from HARPS Comparison of [OI] 6300Å and OI 6158Å S. Bertran de Lis 1, 2, E. Delgado Mena

More information

The Forbidden Abundance of Oxygen in the Sun

The Forbidden Abundance of Oxygen in the Sun The Forbidden Abundance of Oxygen in the Sun Carlos Allende Prieto and David L. Lambert McDonald Observatory and Department of Astronomy, The University of Texas, Austin, TX 78712-1083, USA and Martin

More information

arxiv: v2 [astro-ph] 27 Jan 2009

arxiv: v2 [astro-ph] 27 Jan 2009 PUBLISHED IN APJL (2009) VOL. 691, L119-L122 Preprint typeset using LATEX style emulateapj v. 03/07/07 ON THE SOLAR NICKEL AND OXYGEN ABUNDANCES PAT SCOTT, 1,2,3 MARTIN ASPLUND, 3,4 NICOLAS GREVESSE 5,6

More information

Open Questions in Solar Neutrinos

Open Questions in Solar Neutrinos Open Questions in Solar Neutrinos Overview of SSM and experiments The solar abundance problem and CN neutrinos Other precision measurement opportunities Wick Haxton Solar νs @ JinPing 9 June 2014 The Standard

More information

Chemical Abundance Analysis of the Symbiotic Red Giants

Chemical Abundance Analysis of the Symbiotic Red Giants Chemical Abundance Analysis of the Symbiotic Red Giants Cezary Ga lan 1, Joanna Miko lajewska 1, and Kenneth H. Hinkle 2 1 N. Copernicus Astronomical Center, Bartycka 18, PL-00-716 Warsaw, Poland 2 National

More information

arxiv:astro-ph/ v1 5 May 2004

arxiv:astro-ph/ v1 5 May 2004 Modelling of Stellar Atmospheres IAU Symposium, Vol. xxx, xxxx N. E. Piskunov, W. W. Weiss, D. F. Gray, eds. New Grids of ATLAS9 Model Atmospheres arxiv:astro-ph/0405087v1 5 May 2004 Fiorella Castelli

More information

Are open clusters chemically homogeneous? Fan Liu

Are open clusters chemically homogeneous? Fan Liu Are open clusters chemically homogeneous? Fan Liu Collaborators: Martin Asplund, David Yong, Sofia Feltzing, Jorge Melendez, Ivan Ramirez August 1 st 2018 Why open clusters are important? Open clusters

More information

The Gaia-ESO Survey: Detailed Abundances in the Globular Cluster NGC 4372

The Gaia-ESO Survey: Detailed Abundances in the Globular Cluster NGC 4372 Highlights of Spanish Astrophysics VIII, Proceedings of the XI Scientific Meeting of the Spanish Astronomical Society held on September 8 12, 2014, in Teruel, Spain. A. J. Cenarro, F. Figueras, C. Hernández-

More information

Tc trends and terrestrial planet formation The case of Zeta Reticuli

Tc trends and terrestrial planet formation The case of Zeta Reticuli Tc trends and terrestrial planet formation The case of Zeta Reticuli Vardan Adibekyan Institute of Astrophysics and Space Sciences E. Delgado-Mena, P. Figueira, S.G. Sousa, N.C. Santos, J.P. Faria, J.I.

More information

The photospheric solar oxygen project: I. Abundance analysis of atomic lines and influence of atmospheric. models

The photospheric solar oxygen project: I. Abundance analysis of atomic lines and influence of atmospheric. models The photospheric solar oxygen project: I. Abundance analysis of atomic lines and influence of atmospheric models Elisabetta Caffau, Hans-G. Ludwig, Matthias Steffen, Thomas R. Ayres, Piercarlo Bonifacio,

More information

Model Atmosphere Codes: ATLAS12 and ATLAS9

Model Atmosphere Codes: ATLAS12 and ATLAS9 Model Atmosphere Codes: ATLAS12 and ATLAS9 Robert L. Kurucz Abstract I present three different treatments of opacity and the corresponding programs: Resolved spectra and SYNTHE; Sampled spectra and ATLAS12;

More information

arxiv:astro-ph/ v1 16 Dec 2004

arxiv:astro-ph/ v1 16 Dec 2004 The Metallicity of Post-T Tauri Stars: A preliminary approach to the understanding of the metal enrichment of stars harboring planets arxiv:astro-ph/0412398v1 16 Dec 2004 Ramiro de la Reza, Licio da Silva

More information

Line formation in solar granulation

Line formation in solar granulation Astronomy & Astrophysics manuscript no. (will be inserted by hand later) Line formation in solar granulation IV. [O I], O I and OH lines and the photospheric O abundance Martin Asplund 1, Nicolas Grevesse

More information

Solar Abundances N Grevesse, A J Sauval. Encyclopedia of Astronomy & Astrophysics P. Murdin

Solar Abundances N Grevesse, A J Sauval. Encyclopedia of Astronomy & Astrophysics P. Murdin eaa.iop.org DOI: 10.1888/0333750888/1979 Solar Abundances N Grevesse, A J Sauval From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2005 ISBN: 0333750888 Institute of Physics Publishing

More information

Studying stars in M31 GCs using NIRI and GNIRS

Studying stars in M31 GCs using NIRI and GNIRS Studying stars in M31 GCs using NIRI and GNIRS Ricardo Schiavon Gemini Observatory GSM 2012 San Francisco July 19, 2012 Collaborators Andy Stephens (Gemini) Nelson Caldwell (SAO) Matthew Shetrone (HET)

More information

Characterizing Small Planets via Spectroscopy of their Host Stars Johanna Teske in collaboration with

Characterizing Small Planets via Spectroscopy of their Host Stars Johanna Teske in collaboration with Characterizing Small Planets via Spectroscopy of their Host Stars Johanna Teske in collaboration with Robert Wilson, Steven Majewski, Katia Cunha, Verne Smith, Diogo Souto, Chad Bender, Suvrath Mahadevan,

More information

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014

Volatiles in the terrestrial planets. Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Volatiles in the terrestrial planets Sujoy Mukhopadhyay University of California, Davis CIDER, 2014 Atmophiles: Elements I will talk about rock-loving iron-loving sulfur-loving Temperatures in Protoplanetary

More information

Atlas of CMFGEN Models for OB Massive Stars

Atlas of CMFGEN Models for OB Massive Stars PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC, 127:428 436, 2015 May 2015. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Atlas of CMFGEN Models for OB Massive

More information

Name: Cristina Protasio Esparó. From: UAB Universitat Autònoma de Barcelona. martes 25 de marzo de 14

Name: Cristina Protasio Esparó. From: UAB Universitat Autònoma de Barcelona. martes 25 de marzo de 14 Name: Cristina Protasio Esparó From: UAB Universitat Autònoma de Barcelona SUM UP 1. Previous work: Generalization of the stability to convection in non homogeneous solar models. Solar abundance problem:

More information

Meteorites free samples from the solar system

Meteorites free samples from the solar system Meteorites free samples from the solar system It is easier to believe that Yankee professors would lie, than that stones would fall from heaven [Thomas Jefferson, 3rd president of the USA] 2.1 Collection

More information

The atmosphere of Exoplanets AND Their evolutionary properties. I. Baraffe

The atmosphere of Exoplanets AND Their evolutionary properties. I. Baraffe The atmosphere of Exoplanets AND Their evolutionary properties I. Baraffe I) Properties of cool atmospheres: 1) Atmospheric chemistry 2) Main opacity sources 3) Non solar composition 4) Non equilibrium

More information

Planetary Formation OUTLINE

Planetary Formation OUTLINE Planetary Formation Reading this week: White p474-490 OUTLINE Today 1.Accretion 2.Planetary composition 1 11/1/17 Building Earth 2 things are important: Accretion means the assembly of Earth from smaller

More information

Surface abundances of light elements for a large sample of early B-type stars IV. The magnesium abundance in 52 stars a test of metallicity

Surface abundances of light elements for a large sample of early B-type stars IV. The magnesium abundance in 52 stars a test of metallicity Mon. Not. R. Astron. Soc. 358, 193 201 (2005) doi:10.1111/j.1365-2966.2005.08795.x Surface abundances of light elements for a large sample of early B-type stars IV. The magnesium abundance in 52 stars

More information

PoS(NIC XI)301. Andreas Korn. IFA, Uppsala University. Heidelberg,

PoS(NIC XI)301. Andreas Korn. IFA, Uppsala University. Heidelberg, Andreas Korn IFA, Uppsala University Heidelberg, 2010-07-17 Who is this guy? Born in 1972, raised in Marburg, Germany MSc in Astrophysics (1996, U of London) Diploma in Physics (1998, U of Heidelberg)

More information

Substellar Atmospheres II. Dust, Clouds, Meteorology. PHY 688, Lecture 19 Mar 11, 2009

Substellar Atmospheres II. Dust, Clouds, Meteorology. PHY 688, Lecture 19 Mar 11, 2009 Substellar Atmospheres II. Dust, Clouds, Meteorology PHY 688, Lecture 19 Mar 11, 2009 Outline Review of previous lecture substellar atmospheres: opacity, LTE, chemical species, metallicity Dust, Clouds,

More information

Diffusion and helioseismology

Diffusion and helioseismology Diffusion and helioseismology Jørgen Christensen-Dalsgaard Institut for Fysik og Astronomi, Aarhus Universitet & Danish AsteroSeismology Centre (DASC) Eddington (1926): The internal constitution of the

More information

Stars and Stellar Astrophysics. Kim Venn U. Victoria

Stars and Stellar Astrophysics. Kim Venn U. Victoria Stars and Stellar Astrophysics with ngcfht Kim Venn U. Victoria Stellar SWG: Katia Cunha (NOAO), Rolf-Peter Kudritzki (IfA), Else Starkenburg (U. Victoria) Patrick Dufour (U.Montreal) Zhanwen Han (Yunnan

More information

Origin of heavier elements, origin of universe

Origin of heavier elements, origin of universe Origin of heavier elements, origin of universe Like we said earlier It takes higher and higher temperatures to make larger and larger nuclei fuse together What happens when a star cannot maintain fusion

More information

Fundamental stellar parameters & the fine structure of the Low Main Sequence

Fundamental stellar parameters & the fine structure of the Low Main Sequence Fundamental stellar parameters & the fine structure of the Low Main Sequence Luca Casagrande MPA: I. Ramírez, M. Asplund CAUP: J. Meléndez ANU: M. Bessell Casagrande et al. (2010, A&A - in press; arxiv:1001.3142)

More information

HNRS 227 Fall 2006 Chapter 13. What is Pluto? What is a Planet? There are two broad categories of planets: Terrestrial and Jovian

HNRS 227 Fall 2006 Chapter 13. What is Pluto? What is a Planet? There are two broad categories of planets: Terrestrial and Jovian Key Points of Chapter 13 HNRS 227 Fall 2006 Chapter 13 The Solar System presented by Prof. Geller 24 October 2006 Planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune Dwarf Planets Pluto,

More information

Tests of stellar physics with high-precision data from eclipsing binary stars

Tests of stellar physics with high-precision data from eclipsing binary stars Tests of stellar physics with high-precision data from eclipsing binary stars Ignasi Ribas Institut de Ciències de l Espai (CSIC-IEEC, Barcelona) Barcelona, April 2013 Eclipsing binary systems Eclipsing

More information

arxiv:astro-ph/ v1 24 Aug 2001

arxiv:astro-ph/ v1 24 Aug 2001 Chemical Abundances of OB Stars with High Projected Rotational Velocities arxiv:astro-ph/0108395v1 24 Aug 2001 Simone Daflon Observatório Nacional, Rua General José Cristino 77 CEP 20921-400, Rio de Janeiro

More information

THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy

THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS B. Barbuy IAG - Universidade de São Paulo Outline: Interest of studies on Galactic bulge and globulars Data available on metallicity,, kinematics in field

More information

The Composition of the Old, Metal-Rich Open Cluster, NGC 6791

The Composition of the Old, Metal-Rich Open Cluster, NGC 6791 The Composition of the Old, Metal-Rich Open Cluster, NGC 6791 Liz Jensen --- Smith College, REU at IFA, University of Hawaii 2006 Mentor: Ann M. Boesgaard --- Institute for Astronomy, University of Hawaii

More information

New Dimensions of Stellar Atmosphere Modelling

New Dimensions of Stellar Atmosphere Modelling New Dimensions of Stellar Atmosphere Modelling Derek Homeier 1,2 France Allard 1,3 Bernd Freytag 1 1 CRAL/École Normale Supérieure de Lyon 2 Förderkreis Planetarium Göttingen e.v. 3 Institut d Astrophysique

More information

Solar System Abundances of the Elements

Solar System Abundances of the Elements Solar System Abundances of the Elements Katharina Lodders Washington University in St. Louis and McDonnell Center for the Space Sciences NIC 2018 Overview The Elements Abundances Challenges: Solar & Meteoritic

More information

Wed. Aug. 30, 2017 Reading:

Wed. Aug. 30, 2017 Reading: Wed. Aug. 30, 2017 Reading: Reading for Fri.: Wood Ch. 1 (solar system overview) Reading for Wed. Wed. Wood Ch. 6 & 8 (Asteroids & Meteorites, Solar Nebula) Reading for Fri. Sept. 8. Rozel et al. (link

More information

Asteroids February 23

Asteroids February 23 Asteroids February 23 Test 2 Mon, Feb 28 Covers 6 questions from Test 1. Added to score of Test 1 Telescopes Solar system Format similar to Test 1 Missouri Club Fri 9:00 1415 Fri, last 10 minutes of class

More information

DWARFS IN THE LOCAL REGION

DWARFS IN THE LOCAL REGION The Astronomical Journal, 131:3069 3092, 2006 June # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. A DWARFS IN THE LOCAL REGION R. Earle Luck 1 and Ulrike Heiter 2 Received

More information

Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae

Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae Spectral analysis of very hot H-deficient [WCE]-type central stars of planetary nebulae Graziela R. Keller 1 Colaborators: Luciana Bianchi 2 and Walter J. Maciel 1 1 IAG/Universidade de São Paulo 2 The

More information

Chapter 7: From theory to observations

Chapter 7: From theory to observations Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective

More information

AKARI OBSERVATIONS OF BROWN DWARFS. II. CO 2 as Probe of Carbon and Oxygen Abundances in Brown Dwarfs

AKARI OBSERVATIONS OF BROWN DWARFS. II. CO 2 as Probe of Carbon and Oxygen Abundances in Brown Dwarfs AKARI OBSERVATIONS OF BROWN DWARFS. II. CO 2 as Probe of Carbon and Oxygen Abundances in Brown Dwarfs Takashi Tsuji Institute of Astronomy, School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka,

More information

A new extensive library of synthetic stellar spectra from PHOENIX atmospheres and its application to fitting VLT MUSE spectra

A new extensive library of synthetic stellar spectra from PHOENIX atmospheres and its application to fitting VLT MUSE spectra International Workshop on Stellar Spectral Libraries ASI Conference Series, 2012, Vol. 6, pp 71 78 Edited by Ph. Prugniel & H. P. Singh A new extensive library of synthetic stellar spectra from PHOENIX

More information

3D non-lte corrections for the 6 Li/ 7 Li isotopic ratio in solar-type stars

3D non-lte corrections for the 6 Li/ 7 Li isotopic ratio in solar-type stars Mem. S.A.It. Vol. 88, 61 c SAIt 2017 Memorie della 3D non-lte corrections for the 6 Li/ 7 Li isotopic ratio in solar-type stars G. Harutyunyan 1,2, M. Steffen 1, A. Mott 1,2, E. Caffau 3, G. Israelian

More information

FIA0221: Taller de Astronomía II. Lecture 14 Spectral Classification of Stars

FIA0221: Taller de Astronomía II. Lecture 14 Spectral Classification of Stars FIA0221: Taller de Astronomía II Lecture 14 Spectral Classification of Stars Spectral types along the stellar CMD. Oh, Be A Fine Girl Kiss Me! Classification of Stellar spectra: The MK system: strong He+

More information

Chemical abundances of planet-host stars. Results for alpha and Fe-group elements. 1 With probably the only exception being the studies of beryllium

Chemical abundances of planet-host stars. Results for alpha and Fe-group elements. 1 With probably the only exception being the studies of beryllium A&A 404, 715 727 (2003) DOI: 10.1051/0004-6361:20030543 c ESO 2003 Astronomy & Astrophysics Chemical abundances of planet-host stars Results for alpha and Fe-group elements A. Bodaghee 1,N.C.Santos 1,2,

More information

Center-to-limb Variation of Quiet Sun Intensity Contrasts. Alex Feller

Center-to-limb Variation of Quiet Sun Intensity Contrasts. Alex Feller Center-to-limb Variation of Quiet Sun Intensity Contrasts Alex Feller Introduction Analysis of quiet Sun rms intensity contrasts σ(i) / , as a function of limb distance (µ value), and comparison with

More information

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 06 Oct. 09, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)

More information

Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations

Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations Detailed chemical abundances of M-dwarf planet hosts from APOGEE observations Diogo Souto Observatório Nacional - ON/MCTI + Katia Cunha Anibal Verne Smith C. Allende Prieto Garcia Hernandez Olga Zamora

More information

Detection of MeV scale neutrinos and the solar energy paradigm

Detection of MeV scale neutrinos and the solar energy paradigm Journal of Physics: Conference Series PAPER OPEN ACCESS Detection of MeV scale neutrinos and the solar energy paradigm To cite this article: Aldo Ianni 2018 J. Phys.: Conf. Ser. 940 012023 View the article

More information

Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars

Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars Mem. S.A.It. Suppl. Vol. 22, 103 c SAIt 2012 Memorie della Supplementi Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars W. J. Maciel and R. D. D. Costa Astronomy Department

More information

Formation and Evolution of Planetary Systems

Formation and Evolution of Planetary Systems Formation and Evolution of Planetary Systems Meyer, Hillenbrand et al., Formation and Evolution of Planetary Systems (FEPS): First Results from a Spitzer Legacy Science Program ApJ S 154: 422 427 (2004).

More information

STELLAR PARAMETERS OF M DWARFS FROM LOW AND HIGH-RESOLUTION SPECTRA TOGETHER WITH NEW MODEL ATMOSPHERES

STELLAR PARAMETERS OF M DWARFS FROM LOW AND HIGH-RESOLUTION SPECTRA TOGETHER WITH NEW MODEL ATMOSPHERES SF2A 2012 S. Boissier, P. de Laverny, N. Nardetto, R. Samadi, D. Valls-Gabaud and H. Wozniak (eds) STELLAR PARAMETERS OF M DWARFS FROM LOW AND HIGH-RESOLUTION SPECTRA TOGETHER WITH NEW MODEL ATMOSPHERES

More information

Influence of Departures from LTE on Oxygen Abundance Determination

Influence of Departures from LTE on Oxygen Abundance Determination Influence of Departures from LTE on Oxygen Abundance Determination arxiv:1302.1048v1 [astro-ph.sr] 5 Feb 2013 T. M. Sitnova 1,2 L. I. Mashonkina 1, T. A. Ryabchikova 1 1 Institut of Astronomy of RAS, Moscow,

More information

Metallicities in stars - what solar neutrinos can do

Metallicities in stars - what solar neutrinos can do - what solar neutrinos can do Institute for Nuclear and Particle Physics, Technical University Dresden, 01069 Dresden, Germany E-mail: zuber@physik.tu-dresden.de New elemental abundance determinations

More information

Abundance of Elements. Relative abundance of elements in the Solar System

Abundance of Elements. Relative abundance of elements in the Solar System Abundance of Elements Relative abundance of elements in the Solar System What is the origin of elements in the universe? Three elements formed in the first minutes after the big bang (hydrogen, helium

More information

Chemical abundances in solar analogs Ricardo López Valdivia

Chemical abundances in solar analogs Ricardo López Valdivia Chemical abundances in solar analogs Ricardo López Valdivia Dr. Miguel Chávez Dr. Emanuele Bertone Objetive Make a detailed analysis of chemical abundances in G0-G3 main sequence stars (solar analogs)

More information

Astronomy 404 October 9, 2013

Astronomy 404 October 9, 2013 Nuclear reaction rate: Astronomy 404 October 9, 2013 from the tunneling increases with increasing E from the velocity distrib. decreases with increasing E The Gamow peak occurs at energy Energy generation

More information

arxiv: v1 [astro-ph] 6 Mar 2008

arxiv: v1 [astro-ph] 6 Mar 2008 New Evidence for the Solar Oxygen Crisis from Spectro-Polarimetric Observations H. Socas-Navarro High Altitude Observatory, NCAR 1, 3080 Center Green Dr, Boulder, CO 80301, USA arxiv:0803.0990v1 [astro-ph]

More information

arxiv:astro-ph/ v1 29 Nov 2006

arxiv:astro-ph/ v1 29 Nov 2006 A Grid of NLTE Line-Blanketed Model Atmospheres of Early B-type Stars Thierry Lanz arxiv:astro-ph/0611891 v1 29 Nov 2006 Department of Astronomy, University of Maryland, College Park, MD 20742; lanz@astro.umd.edu

More information

Evolutionary models and age determinations Alessandro Bressan International School for Advanced Studies (SISSA) Trieste

Evolutionary models and age determinations Alessandro Bressan International School for Advanced Studies (SISSA) Trieste Evolutionary models and age determinations Alessandro Bressan International School for Advanced Studies (SISSA) Trieste Also L. Girardi (OAPD) P. Marigo (UNIPD) A. Nanni (SISSA) New release of stellar

More information

Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas)

Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas) Astr 5465 March 6, 2018 Abundances in Late-type Galaxies Spectra of HII Regions Offer a High-Precision Means for Measuring Abundance (of Gas) Emission lines arise from permitted (recombination) and forbidden

More information

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight

Comparative Planetology II: The Origin of Our Solar System. Chapter Eight Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 07 Oct. 15, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)

More information

HII regions and massive stars are very valuable tools to measure present-day oxygen abundances across the Universe.

HII regions and massive stars are very valuable tools to measure present-day oxygen abundances across the Universe. Take away messages HII regions and massive stars are very valuable tools to measure present-day oxygen abundances across the Universe. We have improved A LOT in the last decades on the reliability of oxygen

More information

Stars and their properties: (Chapters 11 and 12)

Stars and their properties: (Chapters 11 and 12) Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using

More information

Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83

Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83 Spitzer Infrared Spectrograph (IRS) Observations of Large Magellanic Cloud Planetary Nebula SMP 83 J. Bernard Salas, J. R. Houck, P. W. Morris, G. C. Sloan, S. R. Pottasch, & D. J. Barry ApJS, 154, 271

More information

Astr 1050 Fri., Feb. 24, 2017

Astr 1050 Fri., Feb. 24, 2017 Astr 1050 Fri., Feb. 24, 2017 Chapter 7 & 8: Overview & Formation of the Solar System Reading: Chapters 7 on Solar System Chapter 8: Earth & Terrestrial Planets Reminders: New homework on MA up this afternoon,

More information

PoS(NIC XI)013. Nucleosynthesis and chemical evolution of intermediate-mass stars: results from planetary nebulae

PoS(NIC XI)013. Nucleosynthesis and chemical evolution of intermediate-mass stars: results from planetary nebulae Nucleosynthesis and chemical evolution of intermediate-mass stars: results from planetary nebulae E-mail: maciel@astro.iag.usp.br Roberto D. D. Costa E-mail: roberto@astro.iag.usp.br Thais E. P. Idiart

More information

Observational Astronomy - Lecture 6 Solar System I - The Planets

Observational Astronomy - Lecture 6 Solar System I - The Planets Observational Astronomy - Lecture 6 Solar System I - The Planets Craig Lage New York University - Department of Physics craig.lage@nyu.edu March 23, 2014 1 / 39 The Sun and the Earth The Sun is 23,000

More information

arxiv:astro-ph/ v1 28 Feb 2003

arxiv:astro-ph/ v1 28 Feb 2003 Stellar Rotation Proceedings IAU Symposium No. 215, c 2003 IAU André Maeder & Philippe Eenens, eds. Absolute Wavelength Shifts A new diagnostic for rapidly rotating stars arxiv:astro-ph/0302592v1 28 Feb

More information

Nebular Hypothesis and Origin of Earth s Water

Nebular Hypothesis and Origin of Earth s Water Nebular Hypothesis and Origin of Earth s Water What is the shape of our solar system? A. Spherical: the Sun is in the center, the planets orbit in spherical shells. B. Disc shaped: fat in the center, tapering

More information

arxiv: v1 [astro-ph.sr] 23 May 2016

arxiv: v1 [astro-ph.sr] 23 May 2016 Astronomy & Astrophysics manuscript no. c ESO 1 May 5, 1 An in-depth spectroscopic examination of molecular bands from 3D hydrodynamical model atmospheres I. Formation of the G-band in metal-poor dwarf

More information

Substellar Atmospheres. PHY 688, Lecture 18 Mar 9, 2009

Substellar Atmospheres. PHY 688, Lecture 18 Mar 9, 2009 Substellar Atmospheres PHY 688, Lecture 18 Mar 9, 2009 Outline Review of previous lecture the Kepler mission launched successfully results P < 1 month planets by September 09 giant planet interiors comparison

More information

Nebular Hypothesis and Origin of Earth s Water

Nebular Hypothesis and Origin of Earth s Water Nebular Hypothesis and Origin of Earth s Water What is the shape of our solar system? A. Spherical: the Sun is in the center, the planets orbit in spherical shells. B. Disc shaped: fat in the center, tapering

More information

NEON AND OXYGEN ABSOLUTE ABUNDANCES IN THE SOLAR CORONA

NEON AND OXYGEN ABSOLUTE ABUNDANCES IN THE SOLAR CORONA The Astrophysical Journal, 659:743Y749, 2007 April 10 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. NEON AND OXYGEN ABSOLUTE ABUNDANCES IN THE SOLAR CORONA E. Landi

More information

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.

Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio. More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column

More information

arxiv:astro-ph/ v2 16 May 2005

arxiv:astro-ph/ v2 16 May 2005 What Is The Neon Abundance Of The Sun? John N. Bahcall Institute for Advanced Study, Einstein Drive,Princeton, NJ 08540 arxiv:astro-ph/0502563v2 16 May 2005 Sarbani Basu Department of Astronomy, Yale University,

More information

Dust in the Diffuse Universe

Dust in the Diffuse Universe Dust in the Diffuse Universe Obscuring Effects Chemical Effects Thermal Effects Dynamical Effects Diagnostic Power Evidence for Grains: Chemical Effects Catalyzes molecular hydrogen formation. Depletion

More information

On the relation between stars and their planets

On the relation between stars and their planets On the relation between stars and their planets Nuno C. Santos Centro de Astrofísica, Universidade do Porto Instituto de Astrofísica e Ciências do Espaço Why we stellar parameters are important in exoplanets

More information

Initial Conditions: The temperature varies with distance from the protosun.

Initial Conditions: The temperature varies with distance from the protosun. Initial Conditions: The temperature varies with distance from the protosun. In the outer disk it is cold enough for ice to condense onto dust to form large icy grains. In the inner solar system ice can

More information

arxiv: v1 [astro-ph.sr] 12 Sep 2009

arxiv: v1 [astro-ph.sr] 12 Sep 2009 Submitted to ApJL Preprint typeset using L A TEX style emulateapj v. 08/22/09 THE PECULIAR SOLAR COMPOSITION AND ITS POSSIBLE RELATION TO PLANET FORMATION J. Meléndez 1 Centro de Astrofísica da Universidade

More information

AN INTRODUCTION TO COSMOCHEMISTRY

AN INTRODUCTION TO COSMOCHEMISTRY AN INTRODUCTION TO COSMOCHEMISTRY CHARLES R. COWLEY Professor of Astronomy, University of Michigan CAMBRIDGE UNIVERSITY PRESS Foreword V a % e x i 1 Overview 1 1.1 The Scope of Cosmochemistry 1 1.2 Cosmochemistry

More information

OCN 201: Origin of the Earth and Oceans. Waimea Bay, Jan 2002

OCN 201: Origin of the Earth and Oceans. Waimea Bay, Jan 2002 OCN 201: Origin of the Earth and Oceans Waimea Bay, Jan 2002 Periodic Table of the Elements Noble IA IIA IIIA IVA VA VIA VIIA VIIIA IB IIB IIIB IVB VB VIB VIIB gases H He Li Be B C N O F Ne Na Mg Al Si

More information

arxiv: v1 [astro-ph.sr] 24 Jul 2015

arxiv: v1 [astro-ph.sr] 24 Jul 2015 Preprint February 19, 2018 Compiled using MNRAS LATEX style file v3.0 On line contribution functions and examining spectral line formation in 3D model stellar atmospheres A. M. Amarsi 1 1 Mount Stromlo

More information

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point)

Question 1 (1 point) Question 2 (1 point) Question 3 (1 point) Question 1 (1 point) If the Earth accreted relatively slowly, the heat obtained from the gravitational potential energy would have had time to escape during its accretion. We know that the Earth was already

More information