Presentation is loading. Please wait.

Presentation is loading. Please wait.

Monitoring of the Yellow Hypergiant Rho Cas: Results of the High-Resolution Spectroscopy During 2007 - 2011 V.G. Klochkova (SAO RAS, Nizhnij Arkhyz, Russia)

Published byEllen McCormick Modified over 9 years ago

Similar presentations

Presentation on theme: "Monitoring of the Yellow Hypergiant Rho Cas: Results of the High-Resolution Spectroscopy During 2007 - 2011 V.G. Klochkova (SAO RAS, Nizhnij Arkhyz, Russia)"— Presentation transcript:

1 Monitoring of the Yellow Hypergiant Rho Cas: Results of the High-Resolution Spectroscopy During 2007 - 2011 V.G. Klochkova (SAO RAS, Nizhnij Arkhyz, Russia) I.A. Usenko (Dpt. Of Astronomy, Odessa Naional University, Odessa, Ukraine)

2 Mean features 1) High-mass stars with limiting high luminosity (M v > -8 m ); 2) High rate of mass loss; 3) Dynamical instability in their atmospheres (pulsations); 4) Presence of extensive circuumstellar shells; 5) «Shell episodes» demonstration

3 Hertzsprung-Russel diagram for the brightest stars

4 Mean Parameters = 4.4 mag ; R = 400 - 500 R sun = 501 200 L sun ; Teff = 6500 - 7200 K Mass = 40 M sun Age = 4-6 Myr Spectral Type: Mass loss: K0 - before 1930 2.5 10 -5 M sun - 1955-57 F8 Ia - 1943 2.5 10 -6 M sun - 1959 K-M - 1946-1947 2.5 10 -5 M sun - 1960 F8-G2 Ia0 - now 1.0 10 -4 M sun - now

5 Related objects V509 Cas (HR 8752) Sp. G0 - G5 Ia0 T eff = 4000 K; log g = -2.0; V t = 11.0 km/s (Luck, 1975) T eff = 5478 K; log g = 0.9 (Fry & Aller, 1975) V 766 Cen (HR 5171) Sp. G8 Ia0 T eff = 4893 K; log g = 0.00 [Fe/H] = +0.02 (Warren, 1973) V382 Car (HR 4337) Sp. G0 Ia0 T eff = 5866 K; log g = 0.5; V t = 7.0 km/s; [Fe/H] =+0.05 (Usenko et al., 2011) V1302 Aql (IRC + 10420) Sp. F8 Ia0 OH-maser

6 Observations 6m BTA telescope SAO RAN echelle-spectrograph NES in Nesmit focus with CCD 2048 x 2048 R = 60000; S/N = 100 Spectral ranges: Extraction: 4422 - 5930 A ECHELLE context from MIDAS 4514 - 6014 A Processing: 5208 - 6690 A DECH 20

7 — V brightness curve of Cas (fi.lled symbols) compared in the top panel to the radial velocity curve (dotted line), observed over the past 8.5 yr (1994-2002) (Loebel et al., 2003, ApJ 583, 923)

8 Fragment of Rho Cas spectrum

9 Effective temperature T eff were determined using spectroscopic criteria (Kovtuykh, 2007, MNRAS 378, 617) by the method based on the depth ratios of selected pairs of spectral lines most sensitives to the temperatuures.

10

11 Spectral lines used in analysis 1) Symmetric lines ( in most cases - single moderate intensity lines of metals). 2) Short-wave components of splitted low- excited absorptions. 3) Long-wave components of splitted low- excited absorptions. 4) Neutral hydrogen lines (alpha & beta).

12 List of splitted lines in Rho Cas spectra ---------------------------------------------------------------------- Element Lambda X low, eV ---------------------------------------------------------------------- Ti II 4563.76 1.22 Fe I 5429.70 0.96 Ti II 4571.97 1.57 Fe I 5434.52 1.01 Ba II 4934.08 0.00 Fe I 5446.92 0.99 Fe I 5269.54 0.85 Fe I 5455.62 1.01 Fe I 5328.04 0.92 Ba II 5853.67 0.60 Fe I 5371.49 0.96 Ba II 6141.71 0.70 Fe I 5397.13 0.92 Ba II 6496.90 0.60 Fe I 5405.77 0.99

13 Heliocentrical Radial velocity measurements V r (sym) -symmetric; V r (blue)- short-wave; V r (red) - long-wave; V r (HI) - neutral hydrogen absorptions. ---------------------------------------------------------------------- Date V r (sym) NL V r (blue) NL V r (red) NL V r (HI) ---------------------------------------------------------------------- 09.03.07 -54.4 613 -65.5 12 -34.9 12 -46.5 (B) 10.03.07 -54.9 556 -66.4 17 -34.5 17 -47.4 (B) 20.10.08 -51.1 519 -62.2 12 -37.1 12 -44.6 (A) 30.09.09 -43.2 483 -62.8 12 -37.1 12 -46.2 (A) 01.08.10 -39.2 551 -61.8 11 -32.6 11 -40.2 (B) 24.09.10 -40.1 411 -60.3 11 -33.4 12 -30.2 (A) 13.01.11 -43.7 473 -59.6 11 -32.9 12 -32.6 (A) 13.01.11 -43.8 548 -60.1 12 -33.9 12 -33.4 (A)

14

15 Ba II 6141 A line profile 1-HJD 2454760.2 (6744 K); 2-HJD 2455575.1 (6322 K); 3-HJD 24518.4 (6610 K); 4-HJD 2455464.4 (6044 K); 5-HJD 2455409.5 (5777 K)

16 D2 Na I 5889 A line profile 1-HJD 2454760.2 (6744 K); 2-HJD 2455575.1 (6322 K); 3-HJD 24518.4 (6610 K); 4-HJD 2455464.4 (6044 K); 5-HJD 2455409.5 (5777 K)

17 D2 Na I 5889 A line profile from Loebel et al. (2003)

18 Central Part of H alpha line profiles 1-HJD 2454760.2 (6744 K); 2-HJD 2455575.1 (6322 K); 3-HJD 24518.4 (6610 K); 4-HJD 2455464.4 (6044 K); 5-HJD 2455409.5 (5777 K)

19 H alpha line profiles from Loebel et al. (2003)

20 Dependence of V r measured by absorption core from its residual intensity Dots - separate absorptions of symmetrical lines of metals; squares - short-wave components of splitting absorptions; circles - long-wave ones; cross - HI absorption components; stars - short-wave and long- wave D Na I lines components; dashed line - V sys = -47 km/s

21 Dependence of V r measured by absorption core from its residual intensity Dots - separate absorptions of symmetrical lines of metals; squares - short-wave components of splitting absorptions; circles - long-wave ones; cross - HI absorption components; stars - shor-twave and long- wave D Na I lines components; dashed line - V sys = -47 km/s

22 Dependence of V r measured by absorption core from its residual intensity Dots - separate absorptions of symmetrical lines of metals; squares - short-wave components of splitting absorptions; circles - long-wave ones; cross - HI absorption components; stars - short-wave and long- wave D Na I lines components; dashed line - V sys = -47 km/s

23

24

25

26

27

28

29

30 Atmosphere parameters and metallicity T eff = 6000 K; log g = 0.25; [Fe/H] = +0.05 (Boyarchuk & Lyubimkov, 1983, Izv. Krym. Astroph. Obs 66, 130) [Na/H] = +0.47; log M/M sun = 1.42 (Takeda & Takada-Hidai, 1994, PASJ 46, 395)

31 Chemical Composition Rho Cas V382 Cas Teff = 6174\pm43 K; log g = 1.0; Teff = 5866\pm47 K; log g = 0.5; Vt = 9.30 km/s Vt = 7.00 km/s Element [E/H] Sigma NL [E/H] Sigma NL C I -0.47 0.14 6. -0.55 0.24 16 O I -0.36 0.30 4 -0.50 0.11 3 Na I +0.44 0.09 2 +0.72 0.18 3 Mg I -0.28 0.26 2 +0.33 0.00 1 Si I +0.08 0.15 15 +0.22 0.20 19 S I -0.16 0.26 2 -0.15 0.12 4 Ca I -0.30 0.11 8 -0.07 0.17 7

32 Chemical Composition Rho Cas V382 Cas Teff = 6174\pm43 K; log g = 1.0; Teff = 5866\pm47 K; log g = 0.5; Vt = 9.30 km/s Vt = 7.00 km/s Element [E/H] Sigma NL [E/H] Sigma NL Sc I +0.50 0.06 4 +0.55 0.09 4 Sc II +0.07 0.03 2 +0.08 0.00 1 Ti I +0.09 0.14 17 +0.27 0.24 31 Ti II -0.27 0.06 2 +0.08 0.00 1 V I +0.04 0.19 11 +0.13 0.16 16 V II +0.01 0.00 1 -0.17 0.12 4 Cr I +0.11 0.30 14 +0.19 0.25 32 Cr II -0.26 0.30 4 +0.18 0.00 1 Mn I -0.34 0.17 7 -0.26 0.24 7

33 Chemical Composition Rho Cas V382 Cas Teff = 6174\pm43 K; log g = 1.0; Teff = 5866\pm47 K; log g = 0.5; Vt = 9.30 km/s Vt = 7.00 km/s Element [E/H] Sigma NL [E/H] Sigma NL Fe I -0.08 0.16 98 +0.05 0.18 157 Fe II -0.08 0.11 17 +0.05 0.11 14 Co I -0.13 0.31 8 +0.13 0.30 12 Ni I +0.01 0.22 30 -0.08 0.23 61 Cu I +0.08 0.39 3 -0.11 0.26 3 Zn I +0.07 0.00 1 -0.06 0.36 3 Sr I +1.65 0.00 1 +0.35 0.00 1

34 Chemical Composition Rho Cas V382 Cas Teff = 6174\pm43 K; log g = 1.0; Teff = 5866\pm47 K; log g = 0.5; Vt = 9.30 km/s Vt = 7.00 km/s Element [E/H] Sigma NL [E/H] Sigma NL Y I +1.07 0.00 1 +1.01 0.00 1 Y II +0.34 0.20 2 +0.16 0.24 1 Zr II -0.02 0.15 2 +0.16 0.07 2 La II +0.08 0.74 2 -0.40 0.00 1 Ce II -0.12 0.19 5 +0.01 0.18 7 Pr II +0.15 0.29 3 +0.07 0.33 3 Nd II +0.19 0.18 9 +0.25 0.15 8 Eu II +0.27 0.12 2 +0.06 0.17 2 Gd II -0.05 0.00 1 +0.08 0.00 1

35 Conclusions 1) During 2007-2011 T eff demostrated changes within 5777-6744 K. 2) The field of velocities has been analysed using the most number of single lines (some hundred ones in each spectrum) and splitted lines (about 12 ones on visual range). 3) The field of velocities has changed from date to date. In the single moments we can observe the radial velocity dependence from the residual line depth, i.e. the existence of velocity gradient in stelllar atmosphere.

36 Conclusions 4)In the long-wave components of splitted absorptional -forming region the velocity gradient take place too. At that its value has exceeded 15 km/s for single moments and the speed depended from line depth is the continuation of such dependence for single lines. 5) In the single date we can see the same gradient from short-wave components, but it is marked less and its value is no more 6 km/s.

37 Conclusions 6 ) Long-wave components of splitting absorptions are the usual photospherical ones, their forming region and velocity do not differ from the same for single absorptions. Short-wave components have formed in the circumstellar shell.

38 Conclusions 7) According to carbon, sodium and magnesium content, Rho Cas has gone through dredge-up in the red supergiant stage and is presently evolving blueward. Our [Na/H] = +0.44 dex agrees excellent with theoretical value +0.47 dex for star with mass about 26-30 M sun from Takeda & Takada-Hidai (1994)

Download ppt "Monitoring of the Yellow Hypergiant Rho Cas: Results of the High-Resolution Spectroscopy During 2007 - 2011 V.G. Klochkova (SAO RAS, Nizhnij Arkhyz, Russia)"

Similar presentations

Am/Fm STARS. General properties Teff > 6100 K (o Leo) Teff < about 10000 K (transition area to HgMn stars) Main sequence stars Slow rotation: vsini

Am/Fm STARS. General properties Teff > 6100 K (o Leo) Teff < about K (transition area to HgMn stars) Main sequence stars Slow rotation: vsini
Fluctuations in ISM Thermal Pressures Measured from C I Observations Edward B. Jenkins Princeton University Observatory.

Fluctuations in ISM Thermal Pressures Measured from C I Observations Edward B. Jenkins Princeton University Observatory.
STELLAR SPECTRAL CLASSIFICATION THE FIRST STEP IN QUANTITATIVE SPECTRAL ANALYSIS PART I AND II Ewa Niemczura Astronomical Institute, University of Wrocław.

STELLAR SPECTRAL CLASSIFICATION THE FIRST STEP IN QUANTITATIVE SPECTRAL ANALYSIS PART I AND II Ewa Niemczura Astronomical Institute, University of Wrocław.
EQ: WHAT IS SUNLIGHT?. Photon Absorption and Emission Photon Continuous stream of photons (light) emitted by energized vibrating electrons. Wavelengths.

EQ: WHAT IS SUNLIGHT?. Photon Absorption and Emission Photon Continuous stream of photons (light) emitted by energized vibrating electrons. Wavelengths.
Classification of Stellar Spectra Essentially all stars appear as point sources. Only differences are brightness and spectra. Many differences in spectra.

Classification of Stellar Spectra Essentially all stars appear as point sources. Only differences are brightness and spectra. Many differences in spectra.
Chapter 13 Cont’d – Pressure Effects

Chapter 13 Cont’d – Pressure Effects
Mass Loss from Red Giant Branch (and AGB) Stars in Globular Clusters Andrea Dupree Harvard-Smithsonian Center for Astrophysics AGB Workshop: 20 May 2010.

Mass Loss from Red Giant Branch (and AGB) Stars in Globular Clusters Andrea Dupree Harvard-Smithsonian Center for Astrophysics AGB Workshop: 20 May 2010.
Variability. Learning outcomes Variability classes of long period variables Various time scales of variability phenomena Spectroscopic variability Connection.

Variability. Learning outcomes Variability classes of long period variables Various time scales of variability phenomena Spectroscopic variability Connection.
Stellar Spectra Ay16 Lecture 2 Feb 5, 2008. The Nearest Star SOHO UV Image.

Stellar Spectra Ay16 Lecture 2 Feb 5, The Nearest Star SOHO UV Image.
Center for Stellar and Planetary Astrophysics Monash University Summary prepared by John Lattanzio Abundances in M71.

Center for Stellar and Planetary Astrophysics Monash University Summary prepared by John Lattanzio Abundances in M71.
Nov. 6, 2008Thanks to Henrietta Leavitt Cepheid Multiplicity and Masses: Fundamental Parameters Nancy Remage Evans.

Nov. 6, 2008Thanks to Henrietta Leavitt Cepheid Multiplicity and Masses: Fundamental Parameters Nancy Remage Evans.
The Circumstellar Environments of the Cool Hypergiants: Implications for the Mass Loss Mechanism Roberta M Humphreys University of Minnesota VY CMa NML.

The Circumstellar Environments of the Cool Hypergiants: Implications for the Mass Loss Mechanism Roberta M Humphreys University of Minnesota VY CMa NML.
The Family of Stars Chapter 8:. Organizing the Family of Stars: The Hertzsprung-Russell Diagram We know: Stars have different temperatures, different.

The Family of Stars Chapter 8:. Organizing the Family of Stars: The Hertzsprung-Russell Diagram We know: Stars have different temperatures, different.
Institute for Astronomy and Astrophysics, University of Tübingen, Germany July 5, 2004Cool Stars, Stellar Systems and the Sun (Hamburg, Germany)1 Turning.

Institute for Astronomy and Astrophysics, University of Tübingen, Germany July 5, 2004Cool Stars, Stellar Systems and the Sun (Hamburg, Germany)1 Turning.
Variability of Be Stars: A Key to the Structure of their Circumstellar Environments Anatoly Miroshnichenko University of Toledo Variable Star Meeting 2004.

Variability of Be Stars: A Key to the Structure of their Circumstellar Environments Anatoly Miroshnichenko University of Toledo Variable Star Meeting 2004.
The Nature of Molecules

The Nature of Molecules
Spring School of Spectroscopic Data Analyses 8-12 April 2013 Astronomical Institute of the University of Wroclaw Wroclaw, Poland.

Spring School of Spectroscopic Data Analyses 8-12 April 2013 Astronomical Institute of the University of Wroclaw Wroclaw, Poland.
Periodic Table – Filling Order

Periodic Table – Filling Order
Atmospheric tomography of supergiant stars (starring μ Cep) Alain Jorissen, Sophie Van Eck, Kateryna Kravchenko (Université Libre de Bruxelles) Andrea.

Atmospheric tomography of supergiant stars (starring μ Cep) Alain Jorissen, Sophie Van Eck, Kateryna Kravchenko (Université Libre de Bruxelles) Andrea.
The study of evolutionary changes in intermediate mass magnetic CP stars across the HR diagram Evgeny Semenko Special Astrophysical Observatory of the.

The study of evolutionary changes in intermediate mass magnetic CP stars across the HR diagram Evgeny Semenko Special Astrophysical Observatory of the.

Similar presentations

Ads by Google