Stellar Oscillations in Giant Stars 1.K giants 2.Mira 3.RV Tau stars

K giants occupy a „messy“ region of the H-R diagram Progenitors are higher mass stars than the sun Giant stars are A-K starts that have evolved off the main sequence and on to the giant branch

A 2 M סּ star on the main sequence Giant stars are of particular interest to planet hunters. Why? Because they have masses in the range of 1-3 M סּ Stars of higher mass than the Sun are ill-suited for RV searches. However the problem with this is getting a good estimate for the mass of the star A 2 M סּ star on the giant branch

The story of variability in K giant stars began in 1989: Smith et al found a 1.89 d period variation in the radial velocity of Arcturus:

1989 Walker et al. Found that RV variations are common among K giant stars These are all IAU radial velocity standard stars !!! Inspired by the Walker et al. Paper, Hatzes & Cochran began a radial velocity survey of a small sample of K giant stars.

The Long Period Variability: Planets?

Hatzes & Cochran surveyed 12 K giants with precise radial velocity measurements and found significant period

Many showed RV variations with periods of days The „3 Muskateers“

The nature of the long period variations in K giants Three possible hypothesis: 1.Pulsations (radial or non-radial) 2. Spots (rotational modulation) 3. Sub-stellar companions

What about radial pulsations? Pulsation Constant for radial pulsations: Q = P M MסּMסּ () 0.5 R RסּRסּ () –1.5 For the sun: Period of Fundamental (F) = 63 minutes = days (using extrapolated formula for Cepheids) Q = P  סּסּ () 0.5 =

What about radial pulsations? K Giant: M ~ 2 M סּ, R ~ 20 R סּ Period of Fundamental (F) = 2.5 days Q = Period of first harmonic (1H) = 1.8 day → Observed periods too long

What about radial pulsations? Alternatively, let‘s calculate the change in radius V = V o sin (2  t/P),  R =2 V o sin (2  t/P) = ∫ 0  /2 VoPVoP   Gem: P = 590 days, V o = 40 m/s, R = 9 R סּ  R ≈ 0.9 R סּ Brightness ~ R 2  m = 0.2 mag, not supported by Hipparcos photometry

What about non-radial pulsations? p-mode oscillations, Period < Fundamental mode Periods should be a few days → not p-modes g-mode oscillations, Period > Fundamental mode So why can‘ t these be g-modes? Hint: Giant stars have a very large, and deep convection zone

Rotation (and pulsations) should be accompanied by other forms of variability 1.Have long lived and coherent RV variations 2. No chromospheric activity variations with RV period 4. No spectral line shape variations with the RV period 3. No photometric variations with the RV period Planets on the other hand:

CFHT McDonald 2.1m McDonald 2.7m TLS The Planet around Pollux (  Gem) The RV variations of  Gem taken with 4 telescopes over a time span of 26 years. The solid line represents an orbital solution with Period = 590 days, m sin i = 2.3 M Jup.

Ca II H & K core emission is a measure of magnetic activity: Active star Inactive star

Ca II emission variations for  Gem If there are no Ca II variations with the RV period, it probably is not activity

Hipparcos Photometry If there are no photometric variations with the RV period, spots on the surface are not causing the variations.

Test 2: Bisector velocity From Gray (homepage) Spectral Line Bisectors For most phenomena like spots, surface structure, or stellar pulsations, the radial velocity variations are all accompained by changes in the shape of the spectral lines. Planets on the other hand cause an overall Doppler shift of the line without an accompanying change in the lines. Spectral line bisectors are a common way to measure line shapes

The Spectral line shape variations of  Gem.

Period590.5 ± 0.9 d RV Amplitude40.1 ± 1.8 m/s e0.01 ± a1.9 AU Msin i2.9 M Jupiter The Planet around  Gem M = 1.9 M sun [Fe/H] = –0.07 The Star Planets have been found around ~ 30 Giant stars

Frink et al P = 1.5 yrs M = 9 M J The Planet around  Dra

From Michaela Döllinger‘s thesis M sin i = 3.5 – 10 M Jupiter P = 272 d m = 6.6 M J e = 0.53 M * = 1.2 M סּ P = 159 d m = 3 M J e = 0.03 M * = 1.15 M סּ P = 477 d m = 3.8 M J e = 0.37 M * = 1.0 M סּ P = 517 d m = 10.6 M J e = 0.09 M * = 1.84 M סּ P = 657 d m = 10.6 M J e = 0.60 M * = 1.2 M סּ P = 1011 d m = 9 M J e = 0.08 M * = 1.3 M סּ JD RV (m/s)

 Tau

Period653.8 ± 1.1 d RV Amplitude133 ± 11 m/s e0.02 ± 0.08 a2.0 AU Msin i10.6 M Jupiter The Planet around  Tau M = 2.5 M sun [Fe/H] = –0.34 The Star

 Dra

Period712 ± 2.3 d RV Amplitude134 ± 9.9 m/s e0.27 ± 0.05 a2.4 Msin i13 M Jupiter The Planet around  Dra M = 2.9 M sun [Fe/H] = –0.14 The Star

Setiawan et al The evidence supports that the long period RV variations in many K giants are due to planets…so what? K giants can tell us about planet formation around stars more massive than the sun. The problem is the getting the mass. This is where stellar oscillations can help.

And now for the stellar oscillations…

Hatzes & Cochran 1994 Short period variations in Arcturus consistent with radial pulsations n = 1 (1H) n = 0 (F)

 Ari velocity variations: Alias n≈3 overtone radial mode

Photometry of  UMa with WIRE guide camera (Buzasi et al. 2000) Equally spaced modes in frequency → p- modes. Observed  = 2.94  Hz

Buzasi et al get a mean spacing of 2.94  Hz and a lowest frequency mode of 1.82  Hz (P = 6.35 d).  UMa has an interferometric radius of 28 R סּ The Fundamental radial mode is given by: 0 ≈0 ≈ 135 M 1/2 R 3/2  Hz Q = P 0 √  /  סּ Where the pulsation constant Q = – 0.116, so P = 2.8, to 8.6 days, if M ≈ 4 M סּ, close to the first frequency. But… Based on the known radius and observed spacing, this gives M ≈ 10 M סּ. So actual spacing may be one-half as a large and one is not seeing all modes (odd or even radial order, n)

 Dra

 Dra : June 1992

 Dra : June 2005

 Dra The short period variations of  Dra can also be explained by radial pulsations, but only n order modes?

 Dra: A planet hosting K giant P 1 = 7 hrs A 1 = 5 m/s P 2 = 6.4 hrs A 2 =6.35 m/s P 3 = 5.9hrs d A 3 =4 m/s 1 = 39.7  Hz 2 = 43.4  Hz 2 = 47.8  Hz Mean  = 4.05  Hz

Recall our Scaling Relations max = M/M סּ (R/R סּ ) 2 √T eff /5777K Frequency spacing: 3.05 mHz 0 ≈0 ≈ 135 M 1/2 R 3/2  Hz n, l =   (n + l/2 +  R ≈ (  mHz  max /3.05 )(135/   Hz  ) 2 Thes can be solved for the radius of the star:

max ≈ 40  Hz (max peak at P = 7 hrs) = 0.04 mHz Mean  = 4.05  Hz We have two cases: 1. These are nonradial modes and the observed spacing is one-half the large spacing 2. These are radial modes and the observed spacing is the large spacing We have 2 equations and 2 unknowns, these can be solved for M, R Case 2: R = 14.5 R סּ M = 2.9 M סּ Case 1: R = 3.6 R סּ M = 0.17 M סּ Case 1 is in disagreement with evolutionary tracks (they cannot be that wrong!) and Hipparcos distance. Conclusion: this is a giant star and we are detecting radial modes.

Stellar Oscillations in  Gem Nine nights of RV measurements of  Gem. The solid line represents a 17 sine component fit. The false alarm probability of these modes is < 1% and most have FAP < 10 –5. The rms scatter about the final fit is 1.9 m s –1

Amplitude (m/s) Window DFT Velocities

Amplitude in m/s Observed RV Frequencies in  Gem

DFT Fit

The Oscillation Spectrum of Pollux The p-mode oscillation spectrum of  Gem based on the 17 frequencies found via Fourier analysis. The vertical dashed lines represent a grid of evenly-spaced frequencies on an interval of 7.12  Hz

0 ≈0 ≈ 135 M 1/2 R 3/2  Hz 0 ≈0 ≈ 7.12  Hz Inteferometric Radius of  Gem = 8.8 R סּ For radial modes → M = 1.89 ± 0.09 M סּ Frequency Spacing Evolutionary tracks give M = 1.94 M סּ For nonradial modes → M = 7.5 M סּ

MOST Photometry for  Gem For = 87 mHz 2K/  m = 65 km/s/mag

Observed Photometric Frequencies in  Gem

For modes for modes found in both photometry and radial velocity the 2K/  m ratio is consistent with values found for Cepheids (2K/  m ≈ 55) and thus radial pulsators. The Radial Velocity – to – Photometric Amplitude Ratio

HD P = 471 d Msini = 14 M J M * = 3.5 s.m. The first Tautenburg planet:

P = 4.8 days P = 2.4 days HD short period variations For M = 3.5 M סּ R = 38 R F = 4.8 d 2H = 2.7 d

P = 5.8 days Periodogram of RV residuals for  Tau after subtracting the long period orbit

Aldebaran with MOST Period consistent with fundamental radial mode for M = 2.5 M סּ 5.8 days But isochrones give M = 1.2 M סּ → overtone?

MOST:  I/I = = 0.02 mag Radial Velocity 2K ~ 300 m/s 2K/  m ≈ 15 Nonradial? The Radial Velocity – to – Photometric Amplitude Ratio

Radial Velocities of  Boo in Estimates of the mass for Arcturus have been controversial and have ranged from 0.1 to 3 M סּ. Can stellar oscillations resolve this?

P 1 = 3.57 d A 1 =34.7 m/s P 2 = 12.8 d A 2 =27.2 m/s P 3 = 2.08 d A 3 =23.2 m/s P 4 = 2.50 d A 3 =11.5 m/s P 5 = 1.74 d A 5 =6.93 m/s P 6 = 5.77d A 6 =6.23 m/s P 7 = 1.38d A 7 =6.27 m/s P 8 = 1.19d A 8 =5.4 m/s Multi-period Fit

Mean spacing = 1.16  Hz The Oscillation Spectrum of Arcturus?

Mozurkowich et al. 2003: Limb darkened diameter = mas = R סּ  = 1.16  Hz → 1.24 M סּ for radial modes  = 2.32  Hz → 5 M סּ for nonradial modes The higher mass is inconsistent with the spectroscopic analysis which indicate M ≈ 1 M סּ

 Boo in 2005 P = 3.36d At any given time not all modes are visible → need lots of observing time over a very long time base → CoRoT and Kepler

A new planet hosting K giant star: 11 UMa P = 657 d Msini = 3.6 M Jupiter e = 0.6 Döllinger et al. In preparation

M * = 1.2 M סּ R * = 36.3 R סּ P 1 = 4.1 d P 2 = 3.1 d P 3 = 7.1 d Consistent with fundamental and low overtone radial modes Oscillations in 11 UMa in 2007

M * = 1.2 M סּ R * = 36.3 R סּ P 1 = 6.2 d P 2 = 14.2 d F = 10.8 d 1H = 6.2 d 2H = 4.1 d 3H = 3.7 d Oscillations in 11 UMa in 2009 We need a radius!

 Oph: G9.5 III (de Ridder et al. A&A 448, , 2006)

Amplitude Spectra of  Oph

Best Fitting Models for  Oph

Radial or Nonradial pulsations? So far we have seen evidence for radial pulsations in K giants, but are there nonradial modes? Two tales of the same star,  Oph

MOST Photometry of  Oph

This power spectrum is typical for giants. You have a Gaussian envelope of excess power due to the p-mode oscillations, and an exponential rise to low frequencies believed to be due to convection motion.

Conclusion: Mean spacing of 5.3  Hz which are radial modes of short lifetime (~3 days). The autocorrelation function shows peaks at possible frequency spacings

Conclusion using the same data set: radial and nonradial modes but with a long (10-20 d) lifetime. The model reproduces  Oph position in the HR diagram and the interferometric radius Echelle diagram for  Oph

So why did two different groups get different answers using the same data set? The answer lies in how you interpret the wings of a peak in the power spectrum. The lifetime of a mode is not infinite and damping results in each mode being split into a number of peaks under a Lorentzian profile whose full width at half maximum (FWHM) is given by:  = 1   = lifetime of mode L(x,  ) =  (  2 +  2 ) The shorter the mode lifetime, the broader the Lorentzian.

Barban et al. Smoothed the power spectrum and intepreted the broad wings around each peak as due to a short lifetime modes. Kallinger at al. Intepreted the wings as being individual modes that were quite narrow in width, ie. that had long lifetimes So who is correct? We will have to wait for CoRoT and Kepler!

Stellar Oscillations in HD (K2III) Observerved with MOST (Kallinger et al. 2008, CoAst.153, 84K)

The Observed Frequencies

The Echelle Diagram and Best Fit Model Conclusion: Photometric space-based observations show evidence for radial and non-radial modes in giant stars

Mira Variables Red Giant Stars Mass less than 2 solar masses Pulsating in periods longer than 100 days Light amplitudes greater than 1 magnitude Short History from Dorrit Hoffleit David Fabricius (1564_1617), an amateur astronomer and native of Friesland, The Netherlands, is recognized as the first to have discovered a long period variable in 1596, later called o (omicron) Ceti by Johann Bayer in Fabricius (Wolf 1877) observed the star from August 3, when he had used it as a comparison star for the determination of the position of the planet he assumed to be Mercury (later identified by Argelander, 1869, as more probably Jupiter), until August 21, when it had increased from magnitude 3 to magnitude 2. In September it faded, disappearing entirely by October (Clerke 1902). At the time Fabricius assumed the star was a nova. However, he observed it to reappear on February 15, Although Pingré saw it October 14, 1631, the star was practically forgotten until Johann Fokkens Holwarda (1618_1651), also of Friesland, rediscovered it in 1638 and determined its period as eleven months. Johannes Hevelius of Danzig (1611_1687) also observed the star on November 7, 1639, and in 1642 named it Mira, "The Wonderful." Fabricius unfortunately did not live to enjoy this appreciation for his discovery. Fabricius, a minister, had been murdered by a peasant whom he had cited from the pulpit as having stolen one of the minister's geese (Poggendorff 1863)!

Light curve of Mira Variables

Joy, 1926: Velocity and Light Curves for Mira from 1926 Integrating the radial velocity curve, the change in radius of the star is ~70 R סּ, or 0.33 AU!

Radial velocity curves of some Mira variables. 2K (peak to peak amplitude): 4 km/s  V ≈ 1 mag 2K/  m ~ 2-3, significantly different from Cepheids

From I.S. Glass: Miras in the LMC Miras do not show an obvious Period – Luminosity Relationship in the Optical, but a clear one in the Infrared A Period-Luminosity Relationship for Miras

Mira is not a symmetric star! Asymmetry is most likely related to non-symmetric mass loss coupled to the pulsations

RV Tau Variables Spectral Type G-K giants (F-G at minimum, G-K at maximum) Pulsating in periods days Light amplitudes 0.2 magnitudes or greater Stars in transition between the AGB and white dwarf stars

Red Giant Branch (RGB) star leaves the main sequence and ascends the giant branch Asymptotic Giant Branch (AGB): After core burning He (horizontal branch stars), the star moves back up the giant branch

RV Tau Variables in the HR Diagram

Oscillations in the M supergiant Betelgeuse (  Ori)

3D simulation of convection in a Ori

Convection cells on a supergiant are large, only a few cells at any given time, whereas the sun has millions (size~700 km). These cells are also long-lived (years)

RV Measurements from McDonald AVVSO Light Curve

Period of  Ori abruptly changed from 317 days to 714 days. This coincided with an abrupt drop in the brightness of  Ori. Fourier transform of red points: Fourier transform of blue points:

 Ori has dust shells surrounding it. These shells may be related to these incidents of changing pulsation modes.

v osc = L/L סּ M/M סּ (23.4 ± 1.4) cm/sec max = M/M סּ (R/R סּ ) 2 √T eff /5777K 3.05 mHz How well do the Scaling Relationships do? StarPeriodV osc MRLV pred P pred  Gem 3.2 hrs4 m/s m/s3.7 hrs  Dra 4 days42 m/s m/s3 d  Ori d 2 km/s km/s174 d Mira330 d6 km/s km/s2370 d In spite of the large range in mass and radius the scaling relationships are reasonably good predictors

 Ori Today we looked at stellar oscillations of stars up the giant branch. In general: Periods get longer, and amplitudes get higher as the star evolves. Most modes are dominated by radial modes. Next week: The stellar graveyard