Pre-main sequence evolution - Revision history

Rebull at 03:57, 2 October 2012

2012-10-02T03:57:28Z

Rebull at 20:13, 17 May 2012

2012-05-17T20:13:45Z

Rebull at 20:10, 17 May 2012

2012-05-17T20:10:46Z

Rebull at 20:06, 17 May 2012

2012-05-17T20:06:10Z

Rebull at 20:00, 17 May 2012

2012-05-17T20:00:59Z

Rebull at 19:54, 17 May 2012

2012-05-17T19:54:14Z

Rebull at 19:53, 17 May 2012

2012-05-17T19:53:57Z

Rebull at 19:53, 17 May 2012

2012-05-17T19:53:36Z

Rebull: Created page with "left"

2012-05-17T19:34:07Z

Created page with "left"

New page

[[image:ibentracks.png|left]]

← Older revision		Revision as of 03:57, 2 October 2012
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	*Planet formation and migration (what if a big jupiter gets dumped into the convection zone as it approaches the MS?)		*Planet formation and migration (what if a big jupiter gets dumped into the convection zone as it approaches the MS?)
	*Binary formation and interaction with a companion (do most stars form in binaries?)		*Binary formation and interaction with a companion (do most stars form in binaries?)
		+
		+	=Other links=
		+	By no means an exhaustive collection, just what I've stumbled across...
		+	*[http://blogs.discovermagazine.com/badastronomy/2012/09/27/the-life-of-a-star-in-14-minutes/ A nice 15 min summary of stellar evolution]

@@ Line 11: / Line 11: @@
 After the dip in L and veer left (hotter), the star is on a Henyey track (also named for historical reasons). The increase in L corresponds to a structural change, e.g., an increase in size of the radiative core. The additional dip as it's approaching the MS corresponds to more structural changes, e.g. a temporarily convective core as it is getting ready to burn H.  I think some of the structure too comes from burning D and Li, but I've forgotten now if Iben has this in his models, and I can't find it quickly in the paper nor my textbooks.
-Note that the youngest stars are red, and the oldest ones are blue, but that is in a relative sense. Young low mass stars will never be as blue as the MS high mass stars. Lowest mass stars also don't change temperature that much on their approach to the MS.
+Note that the youngest stars are red, and the oldest ones are blue, but that is in a relative sense. Young low mass stars will never be as blue as the MS high mass stars, but their end point is (slightly) bluer than where they started. Lower mass stars don't change temperature that much on their approach to the MS.
 Note that the timescales for this are wildly different. According to this paper's original calculations:

@@ Line 11: / Line 11: @@
 After the dip in L and veer left (hotter), the star is on a Henyey track (also named for historical reasons). The increase in L corresponds to a structural change, e.g., an increase in size of the radiative core. The additional dip as it's approaching the MS corresponds to more structural changes, e.g. a temporarily convective core as it is getting ready to burn H.  I think some of the structure too comes from burning D and Li, but I've forgotten now if Iben has this in his models, and I can't find it quickly in the paper nor my textbooks.
-Note that the youngest stars are red, and the oldest ones are blue, but that is a relative term. Young low mass stars will never be as blue as the MS high mass stars. Lowest mass stars also don't change temperature that much on their approach to the MS.
+Note that the youngest stars are red, and the oldest ones are blue, but that is in a relative sense. Young low mass stars will never be as blue as the MS high mass stars. Lowest mass stars also don't change temperature that much on their approach to the MS.
 Note that the timescales for this are wildly different. According to this paper's original calculations:

← Older revision		Revision as of 20:06, 17 May 2012
Line 28:		Line 28:
	*[http://adsabs.harvard.edu/abs/1994ApJS...90..467D D'Antona & Mazzitelli 1994]		*[http://adsabs.harvard.edu/abs/1994ApJS...90..467D D'Antona & Mazzitelli 1994]
	*[http://adsabs.harvard.edu/abs/2000A%26A...358..593S Siess, Dufour, and Forestini 2000]		*[http://adsabs.harvard.edu/abs/2000A%26A...358..593S Siess, Dufour, and Forestini 2000]
		+	*[http://adsabs.harvard.edu/abs/2009ApJ...702L..27B Baraffe, Chabrier, Gallardo 2009]
		+
		+	Things that make this modelling hard -- getting all of these right (and none of them are static in time for the timescales we are talking about):
		+	*Molecules in the stellar atmosphere (unmeasured lines; only affects lower mass stars)
		+	*Chemical evolution
		+	*Magnetic fields
		+	*Rotation rates
		+	*Differential rotation and other forms of mixing -- how do various things change with radius, AND latitude?
		+	*When does a radiative/convective zone form, and how do things behave at the boundary between these zones?
		+	*Winds
		+	*Interactions with the circumstellar disk
		+	*Accretion at all (how is mass being added to the star and what are the implications for things above)
		+	*Episodic accretion (if the mass is dumped in large quantities all at once, or sifted gently on to the star)
		+	*Planet formation and migration (what if a big jupiter gets dumped into the convection zone as it approaches the MS?)
		+	*Binary formation and interaction with a companion (do most stars form in binaries?)

@@ Line 1: / Line 1: @@
 [[image:ibentracks.png|left]] This figure comes from [http://adsabs.harvard.edu/abs/1965ApJ...141..993I Iben, 1965, ApJ, 141, 993], which is an old paper, but still presents the "big picture" of pre-main-sequence evolution as succinctly as anything else I can find.
-This is a HR diagram, so luminosity is on the y-axis and temperature is on the x-axis, where large T's are on the LEFT. You are used to seeing these for mostly main sequence stars, which is where these tracks END. Stars start at the upper right here. Post-main sequence evolution will carry these stars back to the upper right of the diagram and then around to the upper left and then down to WDs in the lower left (approx.)  For more about post-MS evolution, see, e.g., [http://lcogt.net/siab/ http://lcogt.net/siab/]. This page is about PRE-main sequence evolution.
+This is a HR (Hertsprung-Russell) diagram, so luminosity is on the y-axis and temperature is on the x-axis, where large T's are on the LEFT. You are used to seeing these for mostly main sequence (MS) stars, which is where these tracks END. Stars start at the upper right here. Post-main sequence evolution will carry these stars back to the upper right of the diagram and then around to the upper left and then down to white dwarfs in the (approx.) lower left.  For more about post-MS evolution, see, e.g., [http://lcogt.net/siab/ http://lcogt.net/siab/]. This page, however, is about '''PRE-main sequence evolution'''.
-The numbers at the MS end of the tracks correspond to the mass of the stars modeled here. The 15 Msun object moves right to left on kind of a straight line, and the 0.5 Msun object moves pretty much straight down in the diagram.  All of the tracks stop as soon as H starts burning, so none of these objects are yet burning H. They can (and do!) burn Li and D during these phases.
+The numbers at the MS end of the tracks correspond to the mass of the stars modeled here. The 15 Msun object moves right to left on kind of a straight line, and the 0.5 Msun object moves pretty much straight down in the diagram.  All of the tracks stop as soon as H starts burning, so none of these objects are yet burning H. They can (and do!) burn Li and D during these early phases, because Li and D are far easier to pull apart than it is to squish 2 Hs and 2 neutrons together to make He.
 Each of the numbers on the tracks themselves corresponds to an event along the star's evolution, but, e.g., not all the 1's happen '''at the same time'''; they correspond instead to (roughly) the '''same kind of event''' in each star's life. (They actually correspond to times given in an accompanying table -- see the paper!)
-The straight vertical tracks are called Hayashi tracks (named for historical reasons), and correspond to the entire star being convective. When it starts to develop a radiative core, since the structure changes, the way that energy makes it out of the star changes, so the properties of the star as observed also change. This is why the tracks dip in L and then veer left in the diagram.  Note that low-mass stars never make that transition. Extremely low-mass objects never ignite H, so they spend their whole lives contracting on Hayashi tracks (Jupiter does).  But objects big enough to actually burn H at some point (e.g., stars!) but "small enough" masses still spend their Pre-MS lives completely convective.
+The straight vertical parts of the tracks are called Hayashi tracks (named for historical reasons), and correspond to the entire star being convective. When it starts to develop a radiative core, since the structure changes, the way that energy makes it out of the star changes, so the properties of the star as observed also change. This is why the tracks dip in L and then veer left in the diagram.  Note that low-mass stars never make that transition. Extremely low-mass objects never ignite H, so they spend their whole lives contracting on Hayashi tracks (Jupiter does).  But objects massive enough to actually burn H at some point (e.g., stars!) but "small enough" masses still spend their Pre-MS lives completely convective.  Really massive objects spend very little time completely convective.
-After the dip in L and veer left, the star is on a Henyey track (also named for historical reasons). The increase in L corresponds to an increase in size of the radiative core. The additional dip as it's approaching the MS corresponds to more structural changes, e.g. a temporarily convective core as it is getting ready to burn H.  I think some of the structure too comes from burning D and Li, but I've forgotten now if Iben has this in his models, and I can't find it quickly in the paper nor my textbooks.
+After the dip in L and veer left (hotter), the star is on a Henyey track (also named for historical reasons). The increase in L corresponds to a structural change, e.g., an increase in size of the radiative core. The additional dip as it's approaching the MS corresponds to more structural changes, e.g. a temporarily convective core as it is getting ready to burn H.  I think some of the structure too comes from burning D and Li, but I've forgotten now if Iben has this in his models, and I can't find it quickly in the paper nor my textbooks.
 Note that the youngest stars are red, and the oldest ones are blue, but that is a relative term. Young low mass stars will never be as blue as the MS high mass stars. Lowest mass stars also don't change temperature that much on their approach to the MS.
@@ Line 23: / Line 23: @@
 *1.0 Msun objects never reach a point 8 in this calculation; they get to point 7 at 5x10^7 yrs.
 *0.5 Msun objects never reach a point 7 in this calculation; they get to point 5 at 1.6x10^8 yrs.

← Older revision		Revision as of 19:53, 17 May 2012
Line 1:		Line 1:
−	[[image:ibentracks.png\|left]]	+	[[image:ibentracks.png\|left]] This figure comes from [http://adsabs.harvard.edu/abs/1965ApJ...141..993I Iben, 1965, ApJ, 141, 993], which is an old paper, but still presents the "big picture" of pre-main-sequence evolution as succinctly as anything else I can find.
		+
		+	This is a HR diagram, so luminosity is on the y-axis and temperature is on the x-axis, where large T's are on the LEFT. You are used to seeing these for mostly main sequence stars, which is where these tracks end. Stars start at the upper right here. Post-main sequence evolution will carry these stars back to the upper right of the diagram and then around to the upper left and then down to WDs in the lower left (approx.) For more about post-MS evolution, see, e.g., [http://lcogt.net/siab/]. This page is about PRE-main sequence evolution.
		+
		+	The numbers at the MS end of the tracks correspond to the mass of the stars modeled here. The 15 Msun object moves right to left on kind of a straight line, and the 0.5 Msun object moves pretty much straight down in the diagram. All of the tracks stop as soon as H starts burning, so none of these objects are yet burning H. They can (and do!) burn Li and D during these phases.
		+
		+	Each of the numbers on the tracks themselves corresponds to an event along the star's evolution, but, e.g., not all the 1's happen '''at the same time'''; they correspond instead to (roughly) the '''same kind of event''' in each star's life. (They actually correspond to times given in an accompanying table -- see the paper!)
		+
		+	The straight vertical tracks are called Hayashi tracks (named for historical reasons), and correspond to the entire star being convective. When it starts to develop a radiative core, since the structure changes, the way that energy makes it out of the star changes, so the properties of the star as observed also change. This is why the tracks dip in L and then veer left in the diagram. Note that low-mass stars never make that transition. Extremely low-mass objects never ignite H, so they spend their whole lives contracting on Hayashi tracks (Jupiter does). But objects big enough to actually burn H at some point (e.g., stars!) but "small enough" masses still spend their Pre-MS lives completely convective.
		+
		+	After the dip in L and veer left, the star is on a Henyey track (also named for historical reasons). The increase in L corresponds to an increase in size of the radiative core. The additional dip as it's approaching the MS corresponds to more structural changes, e.g. a temporarily convective core as it is getting ready to burn H. I think some of the structure too comes from burning D and Li, but I've forgotten now if Iben has this in his models, and I can't find it quickly in the paper nor my textbooks.
		+
		+	Note that the youngest stars are red, and the oldest ones are blue, but that is a relative term. Young low mass stars will never be as blue as the MS high mass stars. Lowest mass stars also don't change temperature that much on their approach to the MS.
		+
		+	Note that the timescales for this are wildly different. According to this paper's original calculations:
		+	*point 8 for 15 Msun is 6.2x10^4 yrs
		+	*point 8 for 9 Msun is 1.5x10^5 yrs
		+	*point 8 for 5 Msun is 5.7x10^5 yrs
		+	*point 8 for 3 Msun is 2.5x10^6 yrs
		+	*point 8 for 2.25 Msun is 5.9x10^6 yrs
		+	*point 8 for 1.5 Msun is 1.8x10^7 yrs
		+	*point 8 for 1.25 Msun is 3.0x10^7 yrs.
		+	*1.0 Msun objects never reach a point 8 in this calculation; they get to point 7 at 5x10^7 yrs.
		+	*0.5 Msun objects never reach a point 7 in this calculation; they get to point 5 at 1.6x10^8 yrs.