status and future of n physics
Download
Skip this Video
Download Presentation
Status and Future of n -physics

Loading in 2 Seconds...

play fullscreen
1 / 26

Status and Future of n -physics - PowerPoint PPT Presentation


  • 68 Views
  • Uploaded on

Status and Future of n -physics. What do I talk about?. Motivations Oscillations Status Open Questions Near Future Not so far Future Conclusions. Why are we doing ν -physics?. SM is very successful but it leaves a lot of questions open

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'Status and Future of n -physics' - rangle


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
what do i talk about
What do I talk about?
  • Motivations
  • Oscillations
  • Status
  • Open Questions
  • Near Future
  • Not so far Future
  • Conclusions

Björn Wonsak

why are we doing physics
Why are we doing ν-physics?
  • SM is very successful
  • but it leaves a lot of questions open

(e.g. astrophysical questions, like big bang, matter-antimatter asymmetry, supernovaes, etc.)

we want to understand physics beyond the SM

  • There are two ways to do that:
    • High Energies bigger accelerators
    • Study rare, tiny effects more statistics, lower background

Björn Wonsak

why are we doing physics1
Why are we doing ν-physics?
  • Tiny effect (mn/En)2~(eV/GeV)2=10–18 !
  • Suitable methode: Interferometry
    • Needs coherent source
    • Needs Interference (i.e., large mixing angles)
    • Needs long baseline
  • All this is given us by nature:

Neutrino Interferometry (Oscillations) is a unique tool to study physics at very high scales !!!

Lowest order effect of physics at short distances !!!

Björn Wonsak

what are oscillations
What are ν-oscillations?
  • Flavour eigenstates ne,m,tare not the mass eigenstates n1,2,3

neutrino mixing

Pontecorvo-Maki-Nakagawa-Sakata (PMNS) Matrix:

  • This leads to oscillations between the ne,m,t like in the Kaon system
  • ν must have different masses (not all are massless)
  • Leptonflavour is not strictly conserved

Already beyond the SM !

Björn Wonsak

what are oscillations1
What are ν-oscillations?

propagation determined bymass-eigenstates

source createsflavor-eigenstates

detector seesflavor-eigenstates

v2

τ

v3

W

W

μ

p,n

hadrons

slightly different frequencies→ phase difference changes

Mass eigenstates n2,n3with m2, m3

Flavor eigenstates nm, nt

Björn Wonsak

what are oscillations2
What are ν-oscillations?

Probability to find vτ

Distance x in Losz

  • Oscillation probability

with

experiment needs energy resolution

experiment needs statistics

sin2(2θ)

Losz, Δm2

Björn Wonsak

what are oscillations3
What are ν-oscillations?

Zero for CP

conservation

Three flavour mixing:

3 mixing angles and 1 CP-violating phase

If neutrinos are Majorana particles:

2 additional Majorana-Phases (CPV): α1, α2

Björn Wonsak

slide9
Example for 3 flavour Oscillation probability !

L/E is crucial !

sin2(2q13)

sin2(2q12)

Dm213

Dm212

Björn Wonsak

what do we know
What do we know?
  • Atmospheric neutrinos

Super-Kamiokande

Atmosphärische nBeschleuniger n

Björn Wonsak

what do we know1
What do we know?
  • Solar neutrinos

SNO

KamLAND

Reaktor-n

Solar-n

Mass effects in the sun dominate !

Björn Wonsak

what are oscillations4
What are ν-oscillations?

Three flavour mixing:

3 mixing angles and 1 CP-violating phase

Very different Dm2 in different sectors

Solar and atmospheric oscillations can be regarded as independent

2 flavor discription is sufficient

If neutrinos are Majorana particles:

2 additional Majorana-Phases (CPV): α1, α2

Björn Wonsak

what do we want to know
What do we want to know?

bb0n: claim by Klapdor-Kleingrothaus !

  • Dirac or Majorana ?
  • Absolute mass scale ?
  • How small is θ13 ?
  • CP-violation ?
  • Mass hierarchy ?
  • Verify Ocsillations ?
  • LSND ? Sterile neutrinos ? CPT-violation ?

direct measurement: Katrin aims for mn<0,2eV

Diappearance energyspectra, nt apperance

  • can be adressed by oscillation experiments
  • need specialised experiments

Björn Wonsak

what comes next
What comes next?

NUMI

MINOS

735km

Minos

started this year

Magnetized steel/scintillator calorimeter

  • low E neutrinos (few GeV): nm disappearance experiment
  • 4 x1020 pot/year  2500 nm CC/year
  • compare Det1-Det2 response vs E  in 2-6 years sensitivity to Dm2atm
  • main goal: reduce the errors on Dm223 and sin22q23 as needed for sin22q13measurement

Björn Wonsak

slide15
NC/CC ratio measured

contains four neutrino interactions

Björn Wonsak

slide17
What comes next?

nτ appearance experiment

start end 2006

(search for q13)

Emulsion CloudChamber (ECC)

1,8 kton mass

En≈ 17 GeV

Björn Wonsak

slide18
Basic “cell”

Target Trackers

Pb/Em. target

µ spectrometer

8 cm

8 m

n

Pb/Em. brick

nt

1 mm

Pb

Emulsion

Extract selected brick

technic already used by Donut

nt discovery anno 2000

Emulsion Analysis

Vertex search

Decay search

e/γ ID, kinematics

Electronic detectors

select ν interacting brick

µ ID, charge and p

Björn Wonsak

what comes next1
What comes next?

100-200m

1 km

2 reaktors: 8.4GW Pth

  • Double Chooz

100-200 m

12.7 m3

12.7 m3

Search for θ13: Doppel-CHOOZ Reaktorneutrino experiment (France)

first data taking beginning 2007

Double-Chooz sensitivity for (m2 = 2.0-2.5 10-3 eV2):

sin2(213) < 0.025-0.03, 90% C.L.

Björn Wonsak

slide21
sin2(2q13)

sin2(2q12)

Dm213

Dm212

Double-Chooz

Kamland

Björn Wonsak

what comes next to next
What comes next to next?
  • monitor (beam

direction and intensity)

Same spectrum as SK,

BG measurement

n energy spectrum

and intensity

The first Super-Beam: off-axis T2K, from Tokai to SK

start around 2009

Björn Wonsak

slide23
850km

ne/ne appearance

start about 2011

30kt liquid Scintillator detector

NUMI beam with 6.5 x 1020 pot/yr

With a new Proton Driver, 25 x 1020 pot/yr Superbeam!

Bunch time information used n–physics comes back to surface

16mrad off-axis

Björn Wonsak

slide24
T2K

NOvA

with

Neutrino superbeams

Neutrino superbeams

Björn Wonsak

slide25
for maximal atmospheric mixing

with Dm2≈2,5•10-3 eV2

Björn Wonsak

what have we learned
What have we learned?
  • Smart way to reach high energy scales
  • Already physics beyond the SM
  • A lot of interesting open questions
  • First measurements were highly succesfull

time for precision measurements

  • A new intertesting experiment every year

fast growing knowledge

Björn Wonsak

ad