sign in sign up
<<
Home , Dark nebula, Reflection nebula

Stellar evolution – Part I of III formation

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) The (ISM) • The space between the is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful objects in the sky.

• Why study the ISM? • Dense interstellar clouds are the birth place of stars. • Dark clouds alter and absorb the light from stars behind them. Visible only Visible +

Barnard 68

Example: interstellar “reddening” – visible light (especially short wavelengths) is scattered and absorbed by the cloud. However IR radiation is hardly absorbed at all.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Nebulae • Nebulae are of dust, hydrogen, helium and other ionized gas.

• Three types of nebulae: • Emission (HII region) – a hot star illuminates a gas cloud, excites and/or ionizes the gas, which produces emission lines by de-excitation. • – a star illuminates a gas and dust cloud, the light is reflected (scattered) by the dust. Because blue light is scattered at larger angles than red light, the nebula appears blue (Rayleigh scattering cross-section ∝ 1/l4) • – dense clouds of gas and dust that absorb the visible light from the stars behind. Reflection nebula Dark nebula

Note: a nebula can be an emission and reflection nebula.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Structure of the ISM

Two main types of clouds:

• H I (neutral hydrogen) clouds: • Cold (T ~ 100K) clouds of neutral hydrogen (H I) • Moderate density (n ~ 10 to a few hundred atoms per cm3) • Size: ~ 100 pc

• Hot intercloud medium: • Hot (T ~ a few 1000 K) clouds of ionized hydrogen (H II) • Low density (n ~ 0.1 atoms / cm3) • Gas remains ionized because of very low density

Note: those clouds are stable structure and evolve very slowly.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Probing the cold ISM – the 21-cm H line

• Although dust produces most of the obscuration that is readily noticeable, Hydrogen is the dominant component of the ISM (~70% of total mass) with Helium representing most of the rest. Hydrogen found in ISM: • H I: neutral hydrogen – most of the H in diffuse interstellar medium • H II: ionized hydrogen

• H2: molecular hydrogen

• Unless H I is “illuminated” by a high-energy source (UV radiation), cold H I cannot be revealed by relying on de-excitation of higher energy states.

• One (radio) transition is H I can be detected. It is produced by the reversal of spin of the electron relative to the proton.

• This is a very rare process. The lifetime of the excited state is in the millions of years. But there are many H I atoms!

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) 21-cm [1420 MHz] band – galactic plane

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I)

• The birth of stars is still largely an open question – details unclear about beginnings of star formation: the .

• The protostars are formed from interstellar dust and gas clouds collapsing under gravitational attraction

• But what triggers the original collapse? Recall that the ISM gas clouds are stable (or evolving very slowly). Collapse may be triggered by a shock wave, perhaps produced by a nearby supernova explosion, or perhaps associated with the spiral arms of our Galaxy.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Compressed gas clouds and star formation

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Shocks triggering star formation

• Origin of the shock waves? • Supernovae, novae or other stellar explosions • Stellar winds from hot stars • …

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) formation

Protostar: a contracting mass of gas that represents an early stage in the formation of a star before nucleosynthesis (nuclear fusion) has begun.

• Protostars shines but their energy source is NOT nuclear fusion, but the conversion of gravitational potential energy into heat and light (Helmholtz-Kelvin contraction) when the gas / dust collapses and compresses.

• Using a simplified* model, it is possible to estimate the critical size / mass of a gas

cloud given its temperature T and density r0 over which the gas cloud will collapse. The critical mass is called the Jeans mass and the radius (assuming a spherical cloud) the Jeans length.

5%& ,⁄- 3 3⁄- Jeans mass: !" ≈ '()* 4012 15%& 3⁄- Jeans length: 4" ≈ 40'()*12 *See derivation

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) What is µ? 5%& ,⁄- 3 3⁄- Jeans mass: !" ≈ '()* 4012

• µ is the mean molecular weight is the average mass of a free particle in the gas in units of the mass of the hydrogen atom. This is a weighting factor that takes into account the star composition (and ionization state) )6 4 = )*

• Using X, Y and Z, the mass fractions of H, He and others (”metals”) respectively, one get*: 1 1 1 Neutral: ≅ : + < + > 48 4 = 8

1 3 1 + A Fully ionized: ≅ 2: + < + > 4 4 = ? ? *See derivation

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Exercise

• Determine µn and µi for a typical younger star (X=0.70, Y=0.28, Z=0.02)

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) A simple collapse model

• Very simplified model (no rotation, no magnetic field effect, no outward pressure…)

Collapsing gas cloud • Collapsing gas cloud of initial density r0 is ”free falling” at constant temperature (true when the density is low, clearly incorrect when the density increases significantly) Protostar formation 3% 1 ,⁄- • Free fall timescale: !"" = 32 ()* • Note that the timescale doesn’t depend on the initial size and temperature of the gas cloud. Assuming uniform density, all parts of the cloud will take the same amount of time to collapse.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Not so simple! Of course, this is not so simple! Two examples:

• Conservation of angular momentum – as the cloud contracts, its core starts spinning faster, so rotation plays an important role in the creation of a protostar. Also outflow jets forming transient Herbig Haro objects.

• A gas cloud will contract into clumps, which will become the site of multiple star formation. There are limits to how big a single star can be.

Time

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Exercise

• Calculate the Jean’s mass MJ for the following two clouds:

1. A typical diffuse hydrogen cloud assumed to be entirely composed of H I -19 -3 8 -3 (data: T = 50K, r0 = mHnH = 8.4x10 kg.m using nH = 5x10 m , µ=1).

2. The dense core of a giant (data: T = 10K, r0 = 2mHnH2 = -17 -3 10 -3 3x10 kg.m using nH2 = 10 m , µ=2).

• For (2), Deduce the timescale tFF of free-fall collapse.

• Note: the figure shows the evolution of the collapse following the differential equation derived in class.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Giant molecular gas cloud

Carbon Monoxide (CO) map

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Evolution of a protostar in the H-R diagram

• Eventually, temperatures at protostar core reach 10 million (107) K. Sufficient to start fusion. At this stage, the protostar becomes a star and it joins the (MS).

• Before this, the protostar position on H-R diagram depends on its mass

• Therefore, the final position of the star on the MS also depends on mass

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Evolutionary tracks

• Figure shows tracks of protostars of various masses.

• As protostar collapses, it heats up and moves on the H – R diagram.

• Behavior can be complex!

Birth line: the protostar emerges from his dust cocoon.

Ignition of thermonuclear fusion.

Note: protostars are not red giants, even though they begin their lives in that area of the HR diagram. The normal HR diagrams show positions of stable stars only, not protostars

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Evolutionary tracks • Once the protostar reaches the Main Sequence, it becomes a stable star. – The star’s core has reached 107 K and hydrogen fusion starts – The outward thermal pressure balances the inward gravitational pressure and prevents the star from contracting.

• From that point on, the star remains on the MS quietly “burning” its reserves of Hydrogen.

• The heavier (and hotter) the star, the shorter the time it takes for the protostar to become a star. – Weaker gravity = slow contraction – Weaker gravity / lower mass = small core and higher compression needed to ignite fusion.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Evidence of star formation

T Tauri stars 105 to 107 yr old Still in the forming stage.

• Nebula around S Monocerotis contains many massive, very young stars, including T Tauri stars, which are highly variables and bright in IR.

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I) Globules EGG: • Evaporating Gaseous Globules (“EGG”): newly forming stars exposed by the ionizing radiations from massive stars.

Bok globules: • ~10 to 1000 solar masses • Contracting to form protostars

Fred Sarazin ([email protected]) Physics Department, Colorado School of Mines PHGN324: Stellar evolution (I)