Neutron Star Mergers: Hirschegg 2017

Precision mass measurements
for nuclear astrophysics andneutrino physics studies
Basics of Penning-trap mass spectrometry
Precision atomic/nuclear masses
Astro- and neutrino physics studies
Klaus Blaum
Jan 18th, 2017
Klaus.blaum@mpi-hd.mpg.de

Fields of applications
nuclear structure,
nuclear forces(nuclear) astrophysics, astrochemistry,
production of heavy elements,
atomic and molecular binding energies

H2

particlefundamental interactions and their symmetries,
fundamental constants

PCT

antiparticle

C60

Adapted from H. WilschutWhy measuring atomic masses?

Relative mass precision of 10-9 and below can presently ONLY
be reached by Penning-trap mass spectrometry.

Atomic and nuclear masses
Masses determine the atomic and nuclear binding energies
reflecting all forces in the atom/nucleus.

= N·+Z·+Z·– binding energy

MAtom = N•mneutron + Z•mproton + Z•melectron- (Batom + Bnucleus)/c2
δm/m < 10-10

δm/m = 10-6 – 10-8

How to weigh an atom

νc,1

νc,2

νc,1
νc,2

Storage of ions in a Penning trapBUIon q/mCharge qMass m

The free cyclotron frequency is inverse
proportional to the mass of the ions!
An invariance theorem
saves the day:ωc2 = ω+2+ω-2+ωz2

ωc = qB / mωc = ω+ + ω-L.S. Brown, G. Gabrielse, Rev. Mod. Phys. 58, 233 (1986).

Detection techniques
7T

Destructive
time-of-Flightdetection

Destructive
phase-imagingdetection

R ∝ 1/Tobs

δm/m ≈ 10-90

7T

R ∝ 1/Tobs ∙ ∆φ/2π
δm/m ≈ 10-100

S. Eliseev et al., Phys. Rev. Lett. 110, 082501 (2013)

δm/m ≈ 10-11

Non-destructive
induced image
current detection

4.2 K

S. Sturm et al., Phys. Rev. Lett. 107, 143003 (2011)

ISOLTRAP: A Penning-trap setup at CERN

The ISOLTRAP mass spectrometer
2010

1987

1999
1994
Mukherjee et al., Eur. Phys. J. A 35, 1 (2008)
Wolf et al., Nucl. Instrum. Meth. A 686, 82 (2012)

Masses I

Nuclear magic numbers

CPT, ESR, ISOLTRAP, JYFLTRAP, LEBIT, SHIPTRAP, TITAN, TRIGATRAP

New magic number (N=32) and 3N-forces

Nuclear binding energy Bnucl

S2n (MeV)

T1/2 = ms – s 2MAtom = N•mneutron + Z•mproton + Z•melectron - (BBnuclp/s)/c
atom=+1-10
Yield

One-neutron separation energy S1n
S1n = Bnucl(Z,N) – Bnucl(Z,N-1)

Ca:
A.T. Gallant et al., PRL 109, 032506 (2012)
F. Wienholtz et al., Nature 498, 346 (2013)
K:
M. Rosenbusch et al., PRL 114, 202501 (2015)

Two-neutron separation energy S2nS2n = Bnucl(Z,N) – Bnucl(Z,N-2)

ISOLTRAP (CERN)TITAN (TRIUMF)Masses II

Astrophysics and nucleosynthesis

CPT, CSRe, ESR, ISOLTRAP, JYFLTRAP, LEBIT, SHIPTRAP, TITANThe nucleosynthesis paths
Nuclear masses (binding energies)
determine the paths of the processes.
X-ray bursts

Energysupernovae andEnergyn-star merger

Mass spectrometry for nucleosynthesis
Nuclear masses (binding energies)
determine the paths of the processes.

Nuclear astrophysics studies:
Masses, Half-lifes, Reaction RatesCan beaddressed at
FRIB/FAIR

Masses for nuclear astrophysics
Composition of the outer crust of a neutron star
(T1/2 ~ 200ms)

80 ions in 35 minutes!

δm/mδm/m~ 10-8(< 1-8keV)= 4•10R.
R. WolfWolf etet al.,al., Phys.
Phys. Rev.
Rev. Lett.,
Lett., 110,110, 041101
041101 (2013)(2013)

n-rich Cd masses for r-process studies

D. Atanasov et al., PRL
115, 232501 (2015)

M.R. Mumpower, R. Surman, G.C. Mc-Laughlin,
A. Aprahamian, The impact of individual nuclear
properties on r-process nucleosynthesis,
PPNP 86, 86-126 (2016)

Masses III

Neutrino physics applicationsm(νe) < 2 eV/c2 (95% CL)
BASE, FSU, ISOLTRAP, JYFLTRAP, SHIPTRAP, THe-TRAP, TRIGATRAP

THe-TRAP for KATRIN
A high-precision Q(3T-3He)-value measurement

H → 23He + e − + ν Qlit =18 589.8 (1.2) eV
Qlit =18 592.01(7) eV [E. Myers, PRL (2015)]

31We aim for: δQ(3T3He) = 20 meV
δm/m = 7·10-12∆T < 0.02 K/d at 24°C
∆B/B < 10 ppt / h∆x ≤ 0.1 µm

First 12C4+/16O6+ mass ratio measurement at δm/m = 1.4∙10-11 performed.

The ECHo (163Ho) project
Metallic Magnetic Calorimetry

Q-value of EC in 163Ho

Status in 2014
S. Eliseev et al.,PRL (2015)

Q-value with
δQ<1 eVMasses IV

Test of CPT symmetry

BASE: CERN, GSI, Hannover, Mainz, MPIK, RIKEN

Most stringent baryonic CPT test
Compare charge-to-mass ratios Rof p and p:(q/m)p / (q/m)p = 1.000 000 000 001 (69)
S. Ulmer et al., Nature 524, 196 (2015)

Remarkable:

It is not that easy!
Temperature: T = -270°C
Pressure: p < 4∙10-19 mbar
Storage time: years
Experiment: BASE @ AD/CERN

Thanks
Thank you all for the invitationand your attention!
Email: klaus.blaum@mpi-hd.mpg.de
WWW: www.mpi-hd.mpg.de/blaum/

Max Planck Society

IMPRS-PTFS

Adv. Grant MEFUCO

Helmholtz Alliance