TOF-B\rho Mass Measurements at the NSCL

Tof-B Mass Measurements of Very Exotic Nuclides for Astrophysical Calculations at the NSCL

M Matoš, A Estrade, M Amthor, A Aprahamian, D Bazin, A Becerril, T Elliot, D Galaviz, A Gade, S Gupta, G Lorusso, F Montes, J Pereira, M Portillo, A M Rogers, H Schatz, D Shapira, E Smith, A Stolz and M Wallace National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI, USA
Joint Institute of Nuclear Astrophysics, Michigan State University, East Lansing, MI, USA
Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
Institute of Structure and Nuclear Astrophysics, Department of Physics, University of Notre Dame, South Bend, IN, USA
Oak Ridge National Laboratory, Oak Ridge, TN, USA
Department of Physics, The Ohio State University, Columbus, OH, USA
Los Alamos National Laboratory, Los Alamos, NM, USA
matos@nscl.msu.edu
Abstract

Atomic masses play a crucial role in many nuclear astrophysics calculations. The lack of experimental values for relevant exotic nuclides triggered a rapid development of new mass measurement devices around the world. The Time-of-Flight (TOF) mass measurements offer a complementary technique to the most precise one, Penning trap measurements [1], the latter being limited by the rate and half-lives of the ions of interest. The NSCL facility provides a well-suited infrastructure for TOF mass measurements of very exotic nuclei. At this facility, we have recently implemented a TOF-B technique and performed mass measurements of neutron-rich nuclides in the Fe region, important for r-process calculations and for calculations of processes occurring in the crust of accreting neutron stars.

pacs:
21.10.Dr, 26.50.+x, 26.60.+c, 29.27.Eg

1 Introduction

With a minimum rate requirement of the order of 0.01 particles per second and a measurement time shorter than 1 s, the TOF mass measurements offer a complementary technique to the most precise Penning trap measurements. An entire region of the chart of nuclides can be covered in just one experimental run, producing important data related to astrophysical calculations, tests of mass models, and other nuclear physics applications.

2 Principle of the TOF Mass Measurement Technique

Time-of-Flight mass measurements are based on a precise measurement of the time it takes a charged particle to travel between two points within a magnetic optics system with a magnetic rigidity . The mass of the ion is determined from the equation

(1)

where is the time-of-flight of a particle with mass-to-charge ratio and velocity within the path length . In the relativistic case the expression can be written as

(2)

where is the speed of light.

In reality, precise measurements of the path length and absolute measurements of magnetic rigidity are very difficult. Nevertheless, as the path length and the magnetic rigidity can be considered to be constant for a fixed configuration of the system, the direct relation between the time-of-flight and the mass-to-charge ratio can be found using the nuclides with well known mass values.

A typical beam line with a momentum acceptance of several percent does not fulfil the condition of constant B required for a high precision mass measurement. To overcome this problem, two solutions are adapted at existing TOF mass measurement facilities. A measurement of relative magnetic rigidity by a position measurement at a dispersive plane of the magnetic optics system is used at the SPEG spectrometer at GANIL [2] and at the NSCL TOF-B facility (discussed in this paper). These measurements have to address the Z dependence due to energy losses in a position sensitive detector. The other possibility, applied by TOFI at LANL [3] and IMS at GSI [4], is the use of isochronous mode in magnetic optics. In this case, the ions with higher velocities travel on the longer trajectories in such a way that ions with the same mass-to-charge ratios have the same time-of-flight values independently from their energies. This can be achieved for a non-relativistic case if

(3)

for the full acceptance of the beam line. For relativistic cases a term dependent on a mass-to-charge ratio starts to play an important role;

(4)

and the isochronicity is limited to nuclides within a small range of mass-to-charge ratios. This problem can be alleviated by an improved time-of-flight resolution for non-isochronous particles with decreased magnetic rigidity acceptance [5]. In this case, the statistical uncertainty does not have to suffer from the reduced rate as it is compensated by a better resolution, except for the region of the best isochronicity, where the resolution is not improved with smaller acceptance.

Measurements of the magnetic rigidity were recently reported at GSI for the IMS technique [6]. At the future GSI facility a pair of time-of-flight detectors allowing a velocity measurement has been proposed [7].

All the mentioned techniques are one-turn time-of-flight facilities except for the IMS, which uses a storage ring for multiple TOF measurements. This leads to a significantly better resolution and is important for resolving isomeric contaminants in the TOF spectra.

3 Tof-B Mass Measurement Method at the NSCL

At the NSCL a fast radioactive beam is produced in the A1900 fragment separator [8]. The 58 m long time-of-flight line starts at the A1900 extended focal plane and ends at the focal plane of the S800 spectrograph [9], as shown in Figure 1.

Figure 1: An overview of the facility. The primary relativistic beam is accelerated in the coupled cyclotrons K500-K1200. Radioactive ions are produced by fragmentation and separated in the A1900 fragment separator, where the TOF measurements start. The magnetic rigidity measurements are performed in front of the S800 spectrograph operated with dispersion matched optics. The TOF stop detector is placed at the S800 focal plane together with an ion chamber for energy loss measurement and CRDC detectors for particle tracking.

Fast scintillator detectors provide the timing resolution of =30ps. The relative magnetic rigidity is measured at the momentum dispersive plane by position-sensitive micro-channel plate detectors [10] with a position resolution of =0.3mm. For more details refer to [11].

We also tested the operation of the magnetic optics system in an isochronous mode. A GICO calculation [12] was performed to find an isochronous magnetic optics setting. At the beginning of the experimental run, the isochronous mode was successfully achieved with a TOF resolution of  ps, an improvement over the standard optics with  ps as shown in Figure 2. However, for the TOF corrected with the measured magnetic rigidity a resolution of  ps is achieved in the standard dispersion-matched optics mode. We therefore decided to use the TOF-B technique with standard optics.

Figure 2: Measured TOF values of Ga particles compared with their magnetic rigidities for standard (left panel) and isochronous (right panel) magnetic optics. Projected onto the TOF axis the TOF resolution is  ps and  ps respectively. In the case of standard optics the resolution corrected for the magnetic rigidity is  ps.

4 Mass Measurement of Neutron-Rich Kr Fragmentation Products

In the first TOF-B mass measurement at the NSCL a radioactive ion beam in the region of Fe was produced by fragmentation of a relativistic 100 MeV/u Kr primary beam on a solid Be target. Production targets with thicknesses of 46 mg/cm and 94 mg/cm were alternately used to populate a wide region of the chart of the nuclides in the secondary beam without the need for any change in the experimental settings.

The relative mass resolution of obtained in the experiment allowed the relative statistical uncertainties to be . The systematic errors of the order of in the preliminary analysis are expected to be reduced in the final results. Figure 3 shows the relative experimental uncertainties of mass measurements versus isobaric distance from stability (for details see [13]). The results from this work are compared with other mass measurement techniques. The presented technique has access to more exotic nuclides with the NSCL radioactive beam facility and is competitive with SPEG mass measurements.

Figure 3: Relative experimental uncertainty of mass measurement results versus isobaric distance from stability for each nuclide obtained from [13] for comparison with our recent results. The results from this work are shown with open star symbols.

5 Application to Nuclear Astrophysics

5.1 Astrophysical R-Process Seed Nuclei

One of the leading candidates for the location of the r-process is the high entropy ejecta of Type II supernovae [14, 15]. In this scenario neutrinos not only revive the explosion via heating after the initial shock wave stalls due to the in-falling material of outer layers, but also drive the material neutron-rich with the hardening of the spectra relative to the spectra at later times.

As this neutron rich material initially consisting of neutrons, protons and -particles expands adiabatically and cools, heavy particles are formed by a combination of charged-particle reactions (proton and -captures) and neutron captures. As the temperature decreases, charged-particle reactions freeze-out and a subsequent neutron capture process proceeds if there are enough neutrons remaining.

The resulting abundances, when the charge-particle freeze-out occurs, serve as seeds for the subsequent neutron capture process [16, 17]. The abundances are sensitive to neutron separation energies not only when neutron captures take over but also to determine the initial seed composition. Mass values in the required region of nuclides are partially covered by the experiment discussed in this paper. Figure 4 shows the abundance composition at the moment of charge-particle freeze-out for a case with the entropy of 100 and the initial proton-to-nucleon ratio .

Figure 4: Abundance composition at the moment of charge-particle freeze-out in the high entropy ejecta of a Type II supernova simulation for entropy 100 and proton-to-nucleon ratio . The reaction network is described in [17]. The area, covered in this experiment, is marked.

5.2 Heating of the Accreting Neutron Star Crust and Superburst

Processes occuring after accretion of matter onto neutron stars in binary systems have been related to observables in X-ray binaries. The ashes of the rp-process sink deeper into the crust and the electron chemical potential rises with the increasing density.

A calculation, seeding on a single beta-stable even-even rp-process nuclide, was performed in [18, 19]. Two processes were the primary deep crustal heating sources; pycnonuclear fusion at g/cm, and two-stage electron-capture at densities g/cm that includes cold n-emission to maintain mechanical equilibrium within a Wigner-Seitz cell beyond cold neutron drip density.

New X-ray observations have led to the discovery of superbursts that are roughly 10 times more energetic compared to Type I X-ray bursts [20]. The thermally unstable ignition of C at g/cm was a proposed scenario for superbursts [21, 22], although the heat production in the deep crust would not be sufficient to explain observed superburst recurrence timescales of less than 10 years [23, 24].

The recent calculations of crustal heating using a realistic mix of rp-ashes [25] and including electron capture into excited states followed by a radiative deexcitation predict increased heating and therefore shallower superburst ignition and lower recurrence times between 2–3 years.

The results are very sensitive to the nuclear physics of neutron-rich nuclei up to A=106. In particular masses are needed for electron capture thresholds, heating rates from excited state captures, and the separation energies playing a crucial role in neutron reaction rates. New mass measurements in this region, including the experiment discussed in this paper, are important for the calculation to replace the FRDM mass model values [26] that were used.

6 Conclusions

The mass values in the region covered by this work are crucial for astrophysical calculations such as the investigation of the thermal balance in the crust of accreting neutron stars or the calculation of r-process seeding nuclei.

Experimental masses for neutron-rich nuclides have often been shown to be unreliable [27, 28] and new mass measurements are required.

The technique presented in this work is expected to enable the measurements of nuclides far from stability with relative uncertainties of the order of . This method is now established at the NSCL coupled-cyclotron facility and will be used to measure masses of numerous very exotic nuclides.

References

References

  • [1] Blaum K 2006 Phys. Reports 425 1
  • [2] Mittig W 1997 Annu. Rev. Nucl. Part. Sci. 47 27
  • [3] Wouters J M et al 1985 Nucl. Instrum. Methods240 77
  • [4] Hausmann M et al.2000 Nucl. Instrum. MethodsA446 569
  • [5] Matoš M 2004 Ph.D. Thesis, Justus Liebig Universität Giessen, Germany
    http://geb.uni-giessen.de/geb/volltexte/2004/1582
  • [6] Chen L et al 2006 GSI Scientific Report 2005 141
  • [7] Matoš M 2006 AIP Conf. Proc. 819 164
  • [8] Stolz A et al 2005 Nucl. Instrum. MethodsB241 858
  • [9] Bazin D et al 2000 Nucl. Instrum. MethodsB204 629
  • [10] Shapira D et al 2000 Nucl. Instrum. MethodsA454 409
  • [11] Estrade A, Matoš M et al 2006 Proc. of Int. Symp. Nuclei in the Cosmos IX, PoS(NIC-IX) 092
  • [12] Wollnik H et al 1988 AIP Conf. Proc. 177 74
  • [13] Lunney D 2006 Proc. of Int. Symp. Nuclei in the Cosmos IX, PoS(NIC-IX) 010
  • [14] Cowan J J, Thielemann F-K and Truran J W 1991 Phys. Rep. 208 267
  • [15] Woosley S E and Hoffman R D 1992 Astrophys. J. 395 202
  • [16] Freiburghaus C et al 1999 Astrophys. J. 516 381
  • [17] Farouqi K et al 2007 to be published
  • [18] Haensel P and Zdunik J L 1990 Astron. Astrophys., 227 431
  • [19] Haensel P and Zdunik J L 2003 Astron. Astrophys., 404 L33
  • [20] Kuulkers E 2003 Nucl. Phys. B. Proc. Suppl. 132 466
  • [21] Schatz H, Bildsten L and Cumming A 2003 Astrophys. J. 583 L87
  • [22] Cumming A and Bildsten L 2001 Astrophys. J., 559 L127
  • [23] Wijnands R 2001 Astrophys. J. 554 L59
  • [24] Kuulkers E et al 2004 AIP Conf. Proc. 714 257
  • [25] Gupta S et al 2006 submitted to the Astrophys. J. (Preprint astro-ph/0609828)
  • [26] Möller P et al 1995 At. Data Nucl. Data Tables 59 185
  • [27] Matoš M et al 2005 Proc. Int. Symp. on Exotic Nuclei 2004 (Peterhof, Russia) ed Yu E Penionzhkevich and E A Cherepanov (Singapore: World Scientific) p 90
  • [28] Matoš M et al 2005 Proc. Int. Symp. on Exotic Nuclei 2004 (Peterhof, Russia) ed Yu E Penionzhkevich and E A Cherepanov (Singapore: World Scientific) p 96
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
   
Add comment
Cancel
Loading ...
229106
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description