Presentation is loading. Please wait.

Presentation is loading. Please wait.

Differences of LCDM vs. TeVeS HongSheng Andrews

Similar presentations


Presentation on theme: "Differences of LCDM vs. TeVeS HongSheng Andrews"— Presentation transcript:

1 Differences of LCDM vs. TeVeS HongSheng Zhao @St Andrews

2 N Draco © SDSS

3 In a fair world Gravity  Baryon content
Same Gravity for 105 Msun gas cloud = 105 Msun black hole = 105 suns globular = 105 suns dwarf gal … any density profile Blunt tool

4 Variance in self-gravity despite N1 = N2 =105 !
Unbound at r=200pc Why still Bound?

5 One has only Baryon, One bound by Dark Matter!

6 Does this hold in MOND gravity?
Polarisation halo due to scalar field Applies to all satellites Or real dark halo around some satellites

7 Different Roche Lobes in MOND,Newton,TeVeS, DM,

8 MOND-like gravity (Zhao & Tian 2006)

9 Roche Lobe shape changes with laws of gravity

10

11 External-field effect (EFE) on the small satellite m at distance R

12 Similar Enviornment, Different Territorial Claims

13 Large variance

14 Dark Matter/Baryon Exchange Rate Fluctuates
D/B =? Fornax (10-100) Milky Way (10) Globulars (0-1) Any ratio is possible?

15 Updating Scores LCDM TeVeS
Solar System ? ? Tides on Globulars & dSph Rot. curves HSB/LSB Lensing by Ellipticals/Clusters SNIa/CMB


Download ppt "Differences of LCDM vs. TeVeS HongSheng Andrews"

Similar presentations


Ads by Google