# Where Are the r-modes? Chandra Observations of Millisecond Pulsars

## TL;DR

This study uses Chandra X-ray observations of two millisecond pulsars to set new upper limits on their surface temperatures and r-mode oscillation amplitudes, providing insights into neutron star physics and gravitational wave emission.

## Contribution

First X-ray detection and temperature constraints for PSRs J1640+2224 and J1709, establishing lower r-mode amplitude limits compared to accreting neutron stars.

## Key findings

- Detected both pulsars in X-ray band for the first time.
- Set upper limits on surface temperatures (~3.3-4.7 x 10^5 K).
- Derived r-mode amplitude upper limits (~10^-8 to 10^-7).

## Abstract

We present the results of {\it Chandra} observations of two non-accreting millisecond pulsars, PSRs J1640$+$2224 (J1640) and J1709$+$2313 (J1709), with low inferred magnetic fields and spin-down rates in order to constrain their surface temperatures, obtain limits on the amplitude of unstable $r$-modes in them, and make comparisons with similar limits obtained for a sample of accreting low-mass X-ray binary (LMXB) neutron stars. We detect both pulsars in the X-ray band for the first time. They are faint, with inferred soft X-ray fluxes ($0.3-3$ keV) of $\approx$ $6\times10^{-15}$ and $3\times 10^{-15}$ erg cm$^{-2}$ s$^{-1}$ for J1640 and J1709, respectively. Spectral analysis assuming hydrogen atmosphere emission gives global effective temperature upper limits ($90\%$ confidence) of $3.3 - 4.3 \times 10^5$ K for J1640 and $3.6 - 4.7 \times 10^5$ K for J1709, where the low end of the range corresponds to canonical neutron stars ($M=1.4 M_{\odot}$), and the upper end corresponds to higher-mass stars ($M=2.21 M_{\odot}$). Under the assumption that $r$-mode heating provides the thermal support, we obtain dimensionless $r$-mode amplitude upper limits of $3.2 - 4.8 \times 10^{-8}$ and $1.8 - 2.8 \times 10^{-7}$ for J1640 and J1709, respectively, where again the low end of the range corresponds to lower-mass, canonical neutron stars ($M=1.4 M_{\odot}$). These limits are about an order of magnitude lower than those we derived previously for a sample of LMXBs, except for the accreting millisecond X-ray pulsar (AMXP) SAX J1808.4$-$3658, which has a comparable amplitude limit to J1640 and J1709.